LAST NAME: Carnelli FIRST NAME: Ian BIRTH PLACE: Milano BIRTH DATE: 06.02.1976 AFFILIATION: Politecnico di Milano e-MAIL: ian.carnelli@tiscali.it ARRIVAL DATE: 11.09.2005 DEPARTURE: 16.09.2005 SINGLE ROOM: No DOUBLE ROOM: Yes POSSIBLY SHARED WITH: Genziana Frigo (accompanying) TALK: Yes TITLE: Evolutionary Neurocontrol as a Novel Method for Low-Thrust Gravity Assist Trajectory Optimization ABSTRACT: Combining low-thrust propulsion and gravity assists to enhance deep space missions has proven to be a formidable task. While trajectories generated by methods based on optimal control theory are typically close to the needed initial guess, recently investigated global evolutionary programming techniques often necessitate the successive use of different methods. In this paper, a new method based on evolutionary neurocontrollers is presented. The advantage lies in its ability to explore the solution space autonomously to find optimal trajectories, without an initial guess and without permanent attendance of an expert in astrodynamics. For a Mercury rendezvous problem with a Venus gravity assist, preliminary results are presented. POSTER: No POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Knezevic FIRST NAME: Zoran BIRTH PLACE: Osijek (Croatia) BIRTH DATE: 23.08.1949. AFFILIATION: Astronomical Observatory, Volgina 7, 11160 Belgrade 74, Serbia and Montenegro e-MAIL: zoran@aob.bg.ac.yu ARRIVAL DATE: 11.09.2005. DEPARTURE: 16.09.2005. SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: YES TITLE: Chaotic diffusion in the Veritas asteroid family region ABSTRACT: Veritas asteroid family region is dynamically one of the most complex in the asteroid belt. Many studies of chaotic motion in the resonances that cross the family have been published in recent years, with an aim to understand the dynamical mechanisms at work and establish the age of the family. Starting from the work by Milani and Farinella (1994), who introduced the so-called \'chaotic chronology\' method and gave first estimate of an upper limit to the age of the Veritas asteroid family, through several later upgrades (Knezevic and Pavlovic 2002) of the same approach, to the more recent attempts using different approaches (Knezevic et al. 2002, Nesvorny et al. 2003), all the results indicate an unexpectedly young age for this family. Here we show results of a new study which includes a total of 180 members of the family. We computed the time series of proper elements for all these bodies for up to 100~Myr, and we derived the corresponding Lyapunov exponents and diffusion coefficients. We confirmed the previously suggested splitting of the family in 5 dynamically distinct groups, with particular attention payed to the differences of the two main chaotic strips in terms of the long term diffusion and overlap of the resonant harmonics. Finally, we present two independent estimates of the age of the family, one based on the chaotic diffusion and involving members of the family located in the resonant strips, and the other based on remarkable clustering of the nodal longitudes at an epoch in the past found for a group of family members with regular motion. The two estimates are in fair agreement with each other, and with the 8.3~Myr estimate for the age of Veritas family by Nesvorny et al. (2003). Milani A. and P. Farinella: 1994. Nature 370, 40. Knezevic Z. and R. Pavlovic: 2002. Earth, Moon, Planets 88, 155. Knezevic Z., M. Tsiganis and H. Varvoglis: 2002. In: Asteroids, Comets, Meteors ACM2002., European Space Agency SP-500, 335. Nesvorny, D., W.F. Bottke, H. Levison, and L. Dones: 2003. Astrophys. J. 591, 486. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: fouchard FIRST NAME: marc BIRTH PLACE: paris,france BIRTH DATE: July,4th,1972 AFFILIATION: IASF,CNR e-MAIL: marc.fouchard@obspm.fr ARRIVAL DATE: September,11th,2005 DEPARTURE: September, 16th, 2005 SINGLE ROOM: no DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: yes TITLE: Galactic tide models and mappings. ABSTRACT: The study by pure numerical integration of Galactic tide effects on Oort cloud comets over long time scale lead to large CPU times. In order to get a drastic decrease of the CPU time, we present and compare different models which substitute the numerical integrations. These models are built using two different techniques, formalisms and sets of variables. The results turn out to depend on the technique used to simplify the equations but not on the formalism and the set of variables. Using developments of the solutions of the models, mappings are built allowing to further reduce the CPU time. For the mappings, the set of variables which must be used depends of the values of the cometary semi-major axis and eccentricity. Finally, a computer code using two different mappings and pure numerical integrations is built. This code is used to study an example of transport of comets from the Oort cloud to the solar system. The gain in CPU time and the influence of the radial component is highlighted. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Olle FIRST NAME: Merce BIRTH PLACE: Barcelona BIRTH DATE: 22/August/1960 AFFILIATION: UNiversitat Politecnica de Catalunya e-MAIL: merce.olle@upc.edu ARRIVAL DATE: 11/Sept DEPARTURE: 17/Sept SINGLE ROOM: No DOUBLE ROOM: Yes POSSIBLY SHARED WITH: Esther Barrabes (also participant) TALK: yes TITLE: Horseshoe motion in the restricted three body problem ABSTRACT: In the planar RTBP, the invariant manifolds of the collinear equilibrium point $L_3$, for different values of the mass parameter $\\mu$, give rise to horseshoe motion of different kinds: periodic orbits and homoclinic orbits. We give a mechanism, for $\\mu =0$, that explains the families of horseshoe periodic orbits that exist for $\\mu >0$ and small. Horseshoe periodic motion is also analyzed for any value of $\\mu \\in (0,1/2]$. Finally, we consider the spatial RTBP where bifurcating families of 3D horseshoe periodic orbits and horseshoe invariant tori also exist. POSTER: NO POSTER TITLE: -- ABSTRACT: -- ===================================================== LAST NAME: FU FIRST NAME: Yanning BIRTH PLACE: Nanjing, China BIRTH DATE: Sep 13,1964 AFFILIATION: Purple Mountain Observatory e-MAIL: fyn@pmo.ac.cn ARRIVAL DATE: Sep 11,2005 DEPARTURE: Sep 17,2005 SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: YES TITLE: Frequency analysis and representation of slowly diffusing solutions ABSTRACT: Frequency analysis allows to recover precisely the quasiperiodic expansion of regular KAM solutions of Hamiltonian systems (Laskar, 1990, 2005). In the present paper, we consider the problem of representing the solutions of a differential equation system presenting some small drift, resulting from small dissipation or chaotic behavior. We show that, as for the quasiperiodic solutions, in the case of a solution with a single varying frequency, it is still possible to recover exactly the frequency function. We then introduce a function basis with varying fundamental frequencies for decomposing the considered solutions, and propose a numerical technique for the construction of this basis. Examples show that these decompositions can lead to compact representations. Possible applications to the representation of ephemerides of the solar system bodies are indicated. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Conway FIRST NAME: Bruce BIRTH PLACE: USA BIRTH DATE: 3 April 1952 AFFILIATION: Dept. of Aerospace Engineering, Univ. of Illinois e-MAIL: bconway@uiuc.edu ARRIVAL DATE: Sept 11 DEPARTURE: Sept 17 SINGLE ROOM: DOUBLE ROOM: Y POSSIBLY SHARED WITH: Ms. Jane Alsberg (accompanying) TALK: Yes TITLE: Optimization of Trajectories for Interception or Rendezvous Missions to Near Earth Asteroids ABSTRACT: Optimal trajectories are determined for missions to near-Earth asteroids. Low-thrust electric propulsion is used because of its very high specific impulse. However low-thrust is not well suited for escape from the Earth; it can be done but the time required is prohibitively long. Thus a conventional chemical rocket is used for departure from the Earth to interplanetary space. The continuous optimization problem is formulated as a nonlinear programming problem using the collocation method in which the differential equations of motion are included as nonlinear constraint equations. The numerical optimizer determines the continuous control history for the low-thrust magnitude and the thrust pointing direction and the optimal values of discrete parameters such as the date of departure from Earth, the date of arrival at the asteroid, and the location and direction of the departure impulse from Earth orbit. The use of low-thrust electric propulsion is shown to dramatically decrease the mass of the vehicle at launch for a given payload, or alternatively, dramatically increase the payload mass for a given total spacecraft mass. POSTER: No POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Fouchard FIRST NAME: Marc BIRTH PLACE: Paris, France BIRTH DATE: July, 4th, 1972 AFFILIATION: IASF, CNR, Roma - Italy e-MAIL: fouchard@obs-nice.fr ARRIVAL DATE: September, 11th, 2005 DEPARTURE: September, 16th, 2005 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: Galactic tide models and mappings. ABSTRACT: The study by pure numerical integration of Galactic tide effects on Oort cloud comets over long time scale lead to large CPU times. In order to get a drastic decrease of the CPU time, we present and compare different models which substitute the numerical integrations. These models are built using two different techniques, formalisms and sets of variables. The results turn out to depend on the technique used to simplify the equations but not on the formalism and the set of variables. Using developments of the solutions of the models, mappings are built allowing to further reduce the CPU time. For the mappings, the set of variables which must be used depends of the values of the cometary semi-major axis and eccentricity. Finally, a computer code using two different mappings and pure numerical integrations is built. This code is used to study an example of transport of comets from the Oort cloud to the solar system. The gain in CPU time and the influence of the radial component is highlighted. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: pucacco FIRST NAME: giuseppe BIRTH PLACE: s.elia a pianisi BIRTH DATE: 27/7/56 AFFILIATION: Dipartimento di Fisica - Universita\' di Roma Tor Vergata e-MAIL: pucacco@roma2.infn.it ARRIVAL DATE: 11/16 DEPARTURE: 16/16 SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: YES TITLE: Stability of periodic orbits in galactic potentials ABSTRACT: A survey of the stability properties of periodic orbits in non integrable analytic potentials suitable to describe elliptical galaxies is performed through a normal form analysis. Normal modes stability is determined from the nature of relative equilibria of the reduced systems. The results are compared with the analysis performed with other classical approaches. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: TERRACINI FIRST NAME: SUSANNA BIRTH PLACE: SUTTON AND CHEAM (U.K.) BIRTH DATE: 29/04/1963 AFFILIATION: Dipartimento di Matematica e Applicazioni, Universita\' di Milano Bicocca, Milano e-MAIL: susanna.terracini@unimib.it ARRIVAL DATE: 10/09/2005 DEPARTURE: 17/09/2005 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: Collisions and asymptotics in the N-body problem ABSTRACT: We consider the problem of collisions for various interaction potentials, including the logarithmic one. We present some new results on the asymptotic analysis on collisions and parabolic orbits. We apply the asymptotic estimates in order to rule out the presence of collision for minimal trajectories. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Henrard FIRST NAME: Jacques BIRTH PLACE: Kinshasa (Congo) BIRTH DATE: 04/07/40 AFFILIATION: University of Namur e-MAIL: jacques.henrard@fundp.ac.be ARRIVAL DATE: 11/09/05 DEPARTURE: 17/09/05 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: The rotation of IO ABSTRACT: We develop, in the framework of Hamiltonian mechanics, a theory of the rotation of Io, considered as a rigid body. The theory includes the perturbation due to Jupiter (considered as oblate) and the indirect perturbations due to the other Galilean satellites. In order to describe the orbit of Io around Jupiter, we use the synthetic theory of Lainey (Lainey, 2002), the result of a frequency analysis of a numerically integrated Jovian system. The direct effects of the other Galilean satellites are found to be neglectible. Our theory is consistent, with the rigid body model and with Lainey\'s description of the orbit of Io, at least down to $10^{-6}$ radian ($0.2$ arc-second). We find a mean obliquity of $7.610\\; 10^{-4}$ radian ($157$ arc-second) and the period of the three free librations to be $13.11$ days (free libration in longitude), $155.85$ days (free libration in latitude) and $228.03$ days (free wobble). Fourier series are produced describing, in the body frame, the motion of the polar axis of Jupiter, the motion of the unit vector pointing towards Jupiter and the ``motion of the pole\'\' (the motion of the angular momentum with respect to axis of largest inertia). Free librations (depending on three arbitrary parameters) are also computed. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: belmonte FIRST NAME: cinzia BIRTH PLACE: catanzaro BIRTH DATE: 28/7/77 AFFILIATION: Department of Physics of Rome \"La Sapienza\" e-MAIL: ciaulalunae@hotmail.com ARRIVAL DATE: 11/9 DEPARTURE: 16/9 SINGLE ROOM: DOUBLE ROOM: y POSSIBLY SHARED WITH: TALK: n TITLE: ABSTRACT: POSTER: y POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: marini FIRST NAME: valerio BIRTH PLACE: rome BIRTH DATE: 26/10/1978 AFFILIATION: department of mathematics, university of trento, italy & GNFM e-MAIL: marini@science.unitn.it ARRIVAL DATE: 10/9/2005 DEPARTURE: 17/9/2005 SINGLE ROOM: no DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Sidorenko FIRST NAME: Vladislav BIRTH PLACE: Krasnoyarsk, RUSSIA BIRTH DATE: July 27, 1961 AFFILIATION: Keldysh Institute of Applied Mathematics e-MAIL: sidorenk@spp.keldysh.ru ARRIVAL DATE: Sep. 11 DEPARTURE: Sep 17 SINGLE ROOM: DOUBLE ROOM: yes POSSIBLY SHARED WITH: no matter TALK: yes TITLE: Long-term evolution of the asteroid orbits at the 3:1 mean motion resonance with Jupiter (planar problem) ABSTRACT: We consider the 3:1 mean-motion resonance of the planar elliptic restricted three-body problem (Sun-Jupiter-asteroid). Using the numeric averaging both over the orbital motion and over resonant angle librations/oscillations, we obtained the evolutionary equations, which describe the long-term behaviour of the asteroid\'s argument of pericentre and eccentricity (without any restriction on its value). Then a detailed classification of the possible evolution paths was developed. It significantly generalized the similar results on secular effects in the discussed problem, recently obtained within the scope of the well known Wisdom model (Neishtadt, Sidorenko, 2004). A special attention was given to the very-high-eccentricity asteroidal motion. Being limited to relatively small values of the eccentricity, the Wisdom model did not allow for studying possible transitions from moderate values of the eccentricity (e~0.2-0.3) to the values 0.9-0.95 (Ferraz-Mello, Klafke, 1991). We have demonstrated that, under certain conditions, the existing region of adiabatic chaos can be a place where such transitions are permissible. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: LEMAITRE FIRST NAME: Anne BIRTH PLACE: LIEGE (BELGIUM) BIRTH DATE: 26/10/57 AFFILIATION: Math/FUNDP e-MAIL: Anne.Lemaitre@fundp.ac.be ARRIVAL DATE: 11/09/05 DEPARTURE: 17/09/05 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: The 3:2 spin-orbit resonant motion of Mercury ABSTRACT: Our purpose is to build a model of rotation for a rigid Mercury, involving the planetary perturbations and the non spherical shape of the planet. The purpose is double~: the study of the direct influence of such a model on the motion of a satellite (for space missions like BepiColombo) and the building of a reference for the measurements of the non rigidity (existence and size of a core) of Mercury. Our approach is purely analytical, based on Hamiltonian formalism; we start with a first order basic averaged resonant potential (including $J_2$ and $C_{22}$, and the first powers of the eccentricity and the inclination of Mercury). With this kernel model, we calculate and identify the equilibria (4); we select the present one, and introduce local canonical variables, describing the motion around this 3:2 resonance. We perform a canonical untangling transformation, so to generate three sets of action-angle variables, and identify the three basic frequencies associated with this motion. We reintroduce the neglected terms (higher powers of the eccentricity and variables), the short periodic terms (lost in the averaging process) and the planetary perturbations (Venus and Jupiter), and we calcule (through a Lie triangle of order 2 or 3) the three main corrected frequencies and together, thanks to the Lie generator, the three Complete Euler angles describing the rotation. At any point of the development, we use the software SONYR (written by Rambaux and Bois) so to compare and check our calculations. We try to solve the problem of the choice of initial conditions for the rotation by the introduction of dissipations and frictions, which eliminate (in principle) the so-called free librations. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Tommei FIRST NAME: Giacomo BIRTH PLACE: Lucca BIRTH DATE: 26/03/1978 AFFILIATION: Università di Pisa e-MAIL: tommei@mail.dm.unipi.it ARRIVAL DATE: 11/09 DEPARTURE: 16/09 SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: YES TITLE: Canonical elements for Opik theory ABSTRACT: Opik theory (Opik 1976) deals with planetary close encounters of a small body moving on a planetocentric hyperbola. The usual elements used to study the dynamics of the encounter (Valsecchi et al. 2003) are not canonical. We search for canonical ones: starting from hyperbolic Delaunay elements we derive a set of canonical elements for hyperbolic collision orbits (eccentricity e -> 1+, semi-major axis a fixed) and then we introduce the unperturbed velocity of the small body U and the space covered along the asymptote. An interesting result would be to get a canonical set containing the coordinates on the Target Plane, useful for a complete analysis of the future encounters: we discuss this possibility. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Varin FIRST NAME: Victor BIRTH PLACE: Riga, Latvia BIRTH DATE: 24.03.59 AFFILIATION: Keldysh Institute of Applied Mathematics e-MAIL: varin@keldysh.ru ARRIVAL DATE: 10.09,05 DEPARTURE: 17.09.05 SINGLE ROOM: no DOUBLE ROOM: yes POSSIBLY SHARED WITH: A.D. Bruno TALK: yes TITLE: Two-parametric families of periodic solutions of the restricted three-body problem ABSTRACT: We compute natural families of symmetric periodic solutions (SPS) of the planar circular restricted three-body problem for all values of the mass ratio $\\mu \\in [0,1/2]$. The numerical computations are organized as follows. Starting with a generating family for $\\mu=0$, we compute the family for various fixed values of the mass ratio $\\mu \\in (0,1/2]$. For each SPS we compute its period and two traces, namely, the plane and the vertical ones. Two characteristics of the family, i.e.\\ its intersection with the symmetry plane, are plotted in the three coordinate systems: one global and two local ones related to the primaries. We isolate bifurcations of families, which can be of the two types: (I) an intersection with another family; (II) a self-intersection of the family. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Alexander FIRST NAME: Bruno BIRTH PLACE: Moscow BIRTH DATE: 26.06.40 AFFILIATION: Keldysh Institute of Applyed Mathematics e-MAIL: bruno@keldysh.ru ARRIVAL DATE: 10.09.05 DEPARTURE: 17.09.05 SINGLE ROOM: no DOUBLE ROOM: yes POSSIBLY SHARED WITH: Victor Varin TALK: yes TITLE: Two-parametric families of periodic solutions of the restricted three-body problem ABSTRACT: This is a joint project with V.Varin. We compute natural families of symmetric periodic solutions of the planar circular restricted 3-body problem for $\\mu \\in [0,1/2]$. Preliminary conclusions: 1. Bifurcations of the type (I) are preserved for all $\\mu \\in [0,1/2]$; hence it is sufficient to describe them for $\\mu=0$, i.e.\\, for generating families. 2. Bifurcations of the type (II) are present only for some families of SPS, and for them, these bifurcations may occur for infinite sequence of values of $\\mu$. 3. For small $\\mu$, the behavior of SPS of the first species is in accordance to the current theory of regular perturbations (Bruno A.D. The Restricted 3-Body Problem. de Gruyter: Berlin, 1994). 4. For small $\\mu$, for the SPS of the second species, the plane stability, as a rule, differs from the vertical one; the values of traces are fast decreasing as $\\mu$ grows. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Bruno FIRST NAME: Alexander BIRTH PLACE: Moscow BIRTH DATE: 26.06.40 AFFILIATION: Keldysh Institute of Applyed Mathematics e-MAIL: bruno@keldysh.ru ARRIVAL DATE: 10.09.05 DEPARTURE: 17.09.05 SINGLE ROOM: no DOUBLE ROOM: yes POSSIBLY SHARED WITH: Victor Varin TALK: yes TITLE: Two-parametric families of periodic solutions of the restricted three-body problem ABSTRACT: This is a joint project with V.Varin. We compute natural families of symmetric periodic solutions of the planar circular restricted 3-body problem for $\\mu \\in [0,1/2]$. Preliminary conclusions: 1. Bifurcations of the type (I) are preserved for all $\\mu \\in [0,1/2]$; hence it is sufficient to describe them for $\\mu=0$, i.e.\\, for generating families. 2. Bifurcations of the type (II) are present only for some families of SPS, and for them, these bifurcations may occur for infinite sequence of values of $\\mu$. 3. For small $\\mu$, the behavior of SPS of the first species is in accordance to the current theory of regular perturbations (Bruno A.D. The Restricted 3-Body Problem. de Gruyter: Berlin, 1994). 4. For small $\\mu$, for the SPS of the second species, the plane stability, as a rule, differs from the vertical one; the values of traces are fast decreasing as $\\mu$ grows. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Benet FIRST NAME: Luis BIRTH PLACE: Mexico City BIRTH DATE: 16.09.68 AFFILIATION: Centro de Ciencias Fisicas, National University of Mexico e-MAIL: benet@fis.unam.mx ARRIVAL DATE: 11.09.05 DEPARTURE: 15.09.05 SINGLE ROOM: Yes DOUBLE ROOM: No POSSIBLY SHARED WITH: TALK: Yes TITLE: Title to be anounced ABSTRACT: I have two options of subjects to present, one about narrow planetary rings, and the second on AMD stability. I would like to ask to some time to give the definitive title, because we are getting new result on both subjects, and we would like to choose the nicest to present it. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: FUKUSHIMA FIRST NAME: TOSHIO BIRTH PLACE: FUKUOKA, JAPAN BIRTH DATE: 54/10/27 AFFILIATION: National Astronomical Observatory of Japan e-MAIL: Toshio.FUkushima@nao.ac.jp ARRIVAL DATE: Sept. 10th DEPARTURE: Sept. 17 SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: YES TITLE: Efficient Orbit Integration by Manifold Correction Methods ABSTRACT: Recently we developed a new formulation of numerical integration of perturbed two-body problems named manifold correction methods (Fukushima 2003a, b, c, 2004a, b, c, d, e, f, 2005a, b, c, d). The main trick is to follow the time evolution of some quasi-conserved quantities such as the Kepler energy with the state vector and to maintain rigorously the consistency among them by applying geometric correction such as scaling or rotation at every integration step. The growth of integration errors by the new methods are significantly slower than the standard method. This feature is independent on the type of integrators used or on the kind of perturbations. Also, the manifold correction method is universally realized for the KS-regularized orbits by applying the same method to the perturbed harmonic oscillators. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Waz FIRST NAME: Piotr BIRTH PLACE: Torun (Poland) BIRTH DATE: 03.10.1966 AFFILIATION: Centrum Astronomii, Uniwersytet Mikolaja Kopernika, Gagarina 11, 87-100 Torun, Poland e-MAIL: snake@astri.uni.torun.pl ARRIVAL DATE: 11 September DEPARTURE: 16 September SINGLE ROOM: No DOUBLE ROOM: Yes POSSIBLY SHARED WITH: any nonsmoker male participant TALK: No TITLE: ABSTRACT: POSTER: Yes POSTER TITLE: Dynamics of Planetary and Star Systems Including Perturbing Forces ABSTRACT: In this presentation the influence of the the nonsphericity of the potential on the orbital motion and, as a consequence, on the stability of extrasolar planetary systems is described. A significance of this effects, though in entirely different context (the evolution of the orbit of Phobos, a Moon of Mars) has already been demonstrated [1,2]. The systems of planets of Jupiter type which are close to the star are considered. The construction of an analytical model of the influence of the perturbing forces on the dynamics of the system is attempted. The derived formulas are used in studies of other systems including multiple systems of stars. Acknowledgements This work has been supported by the Polish KBN. References [1] Waz P., Analytical Theory of the Motion of Phobos - Analysis of the Perturbational Function, A&A 348, 300-310, 1999. [2] Waz P., Analytical Theory of the Motion of Phobos - Comparison with Numerical Integration, A&A 416, 1187-1192, 2004. ===================================================== LAST NAME: Kaloshin FIRST NAME: Vadim BIRTH PLACE: Kharkov, Ukraine BIRTH DATE: 12/9/1972 AFFILIATION: California Institute of Technology e-MAIL: kaloshin@its.caltech.edu ARRIVAL DATE: 11 DEPARTURE: 16 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: ABSTRACT: POSTER: No POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: SOUCHAY FIRST NAME: Jean BIRTH PLACE: St. Germain en Laye BIRTH DATE: 14/02/59 AFFILIATION: Observatoire de Paris e-MAIL: Jean.Souchay@obspm.fr ARRIVAL DATE: 11/09 DEPARTURE: 16/09 SINGLE ROOM: DOUBLE ROOM: YES POSSIBLY SHARED WITH: Akémi SOUCHAY TALK: Yes TITLE: Precise determination of the rotation of the asteroid 433 Eros ABSTRACT: Following the NEAR space mission around Eros a large amount of data concerning the physical and dynamical properties of the asteroid could be obtained, from which a very precise analytical modelling of its rotation was possible. We present the results concerning the nutation and the precession of the asteroid, at different time scales. POSTER: No POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Gales FIRST NAME: Catalin Bogdan BIRTH PLACE: Gura Humorului (Romania) BIRTH DATE: 29 July 1976 AFFILIATION: University Al. I. Cuza, Iasi, Faculty of Mathematics e-MAIL: cgales@uaic.ro ARRIVAL DATE: 11 DEPARTURE: 13 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Tsygvintsev FIRST NAME: Alexei BIRTH PLACE: Russia BIRTH DATE: 11/01/75 AFFILIATION: École Normale Supérieure de Lyon e-MAIL: atsygvin@umpa.ens-lyon.fr ARRIVAL DATE: 11/09 DEPARTURE: 16/09 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: CICEK FIRST NAME: Caner BIRTH PLACE: TURKEY BIRTH DATE: 1965 AFFILIATION: Astronomer e-MAIL: canerk@bornova.ege.edu.tr ARRIVAL DATE: 10.09.2005 DEPARTURE: 16.10.2005 SINGLE ROOM: no DOUBLE ROOM: yes POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: yes POSTER TITLE: A near-contact binary CN Andromedae ABSTRACT: New BVR light curves and photometric analysis of the eclipsing binary star CN And are presented. The BVR light curves and radial velocity curves were solved with wilson devinney methods.Orbital period of system was analyzed.Also disscussed the evolution of the system. ===================================================== LAST NAME: Erdem FIRST NAME: Ahmet BIRTH PLACE: TURKEY BIRTH DATE: 1968 AFFILIATION: Astronomer e-MAIL: ardem@physics.comu.edu.tr ARRIVAL DATE: 10.09.2005 DEPARTURE: 16.09.2005 SINGLE ROOM: no DOUBLE ROOM: yes POSSIBLY SHARED WITH: caner cicek TALK: no TITLE: ABSTRACT: POSTER: yes POSTER TITLE: A Near Contact Binary :CN Andromedae ABSTRACT: New BVR light curves and photometric analysis of the eclipsing binary star CN And are presented. The BVR light curves and radial velocity curves were solved with wilson devinney methods.Orbital period of system was analyzed.Also disscussed the evolution of the system. ===================================================== LAST NAME: Erdem FIRST NAME: Ahmet BIRTH PLACE: TURKEY BIRTH DATE: 1968 AFFILIATION: Astronomer e-MAIL: aerdem@physics.comu.edu.tr ARRIVAL DATE: 10.09.2005 DEPARTURE: 16.09.2005 SINGLE ROOM: no DOUBLE ROOM: yes POSSIBLY SHARED WITH: caner cicek TALK: no TITLE: ABSTRACT: POSTER: yes POSTER TITLE: A Near Contact Binary :CN Andromedae ABSTRACT: New BVR light curves and photometric analysis of the eclipsing binary star CN And are presented. The BVR light curves and radial velocity curves were solved with wilson devinney methods.Orbital period of system was analyzed.Also disscussed the evolution of the system. ===================================================== LAST NAME: Falcolini FIRST NAME: Corrado BIRTH PLACE: Roma BIRTH DATE: 17/04/60 AFFILIATION: Universita\' Roma Tre e-MAIL: falco@mat.uniroma3.it ARRIVAL DATE: 11/09/05 DEPARTURE: 16/09/05 SINGLE ROOM: no DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: yes TITLE: Domains of analyticity in four-dimensional maps ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: CACCIANI FIRST NAME: ALESSANDRO BIRTH PLACE: ROME BIRTH DATE: 090138 AFFILIATION: PHYSICS, UNIV. \"LA SAPIENZA\" e-MAIL: alessandro.cacciani@roma1.infn.it ARRIVAL DATE: TBD DEPARTURE: TBD SINGLE ROOM: no DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: YES TITLE: PRECISE MEASUREMENT OF THE SOLAR GRAVITATIONAL RED SHIF ABSTRACT: Using our MOF technology (Magneto-Optical Filter) we are able to improve considerably the current precision (at the level of 2 % as quoted by the last figure given by LoPresto) of the Solar GRS. The project, in collaboration with LoPresto himself, is conceived in two step: 1) from the ground and 2) from the space. This last effort will require precise dtermination of two spacecraft motions, one gloing towards the Sun and the other orbiting around the Earth. The measure is relevant as a test of the General Theory of Relativity. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Pinzari FIRST NAME: Gabriella BIRTH PLACE: Rome BIRTH DATE: 05/21/1966 AFFILIATION: Universita\' Roma Tre, Italy e-MAIL: pinzari@mat.uniroma3.it ARRIVAL DATE: 09/11/2005 DEPARTURE: 09/16/2005 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: Four classical methods for determining planetary elliptic elements: a comparison ABSTRACT: The discovery of the asteroid Ceres by G. Piazzi in 1801 motivated the development of a mathematical technique proposed by C.F.Gauss, which allows to recover the orbit of a celestial body starting from a minimum of three observations. Here we compare the method proposed by Gauss with the techniques (based on three observations) developed by P.S. Laplace and by O.F. Mossotti. We also consider another method developed by O.F.Mossotti, based on four observations. We provide a theoretical and numerical comparison among the different procedures. As an application, we consider the computation of the orbit of the asteroid Juno. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Pinzari FIRST NAME: Gabriella BIRTH PLACE: Rome BIRTH DATE: 05/21/1966 AFFILIATION: Universita\' Roma Tre, Italy e-MAIL: pinzari@mat.uniroma3.it ARRIVAL DATE: 09/11/2005 DEPARTURE: 09/16/2005 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: Four classical methods for determining planetary elliptic elements: a comparison ABSTRACT: The discovery of the asteroid Ceres by G. Piazzi in 1801 motivated the development of a mathematical technique proposed by C.F.Gauss, which allows to recover the orbit of a celestial body starting from a minimum of three observations. Here we compare the method proposed by Gauss with the techniques (based on three observations) developed by P.S. Laplace and by O.F. Mossotti. We also consider another method developed by O.F.Mossotti, based on four observations. We provide a theoretical and numerical comparison among the different procedures. As an application, we consider the computation of the orbit of the asteroid Juno. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Alessi FIRST NAME: Elisa Maria BIRTH PLACE: Padova BIRTH DATE: 19/04/1981 AFFILIATION: Dipartimento di Astronomia - Università di Padova e-MAIL: alessi@pd.astro.it ARRIVAL DATE: 11/09/2005 DEPARTURE: 16/09/2005 SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Zhou FIRST NAME: Ji-Lin BIRTH PLACE: Zhejiang, China BIRTH DATE: Dec.4,1969 AFFILIATION: Professor e-MAIL: zhoujl@nju.edu.cn ARRIVAL DATE: Sept.11 DEPARTURE: Sept.17 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Fu Yan-Ning TALK: YES TITLE: The Stability of Multi-Planet Systems in Large Scale ABSTRACT: We study numerically the stability of multiple planet systems with equal mass and regularly spaced according to their mutual Hill\'s radius. The separations of planets have larger scales as those of our solar system. The time scale T that a system becomes unstable (either orbital crossing or close encounters occur for any two of the planets) can be expressed as a power law, $\\log T= Blog (\\Delta a) +C$, with B and C are constants depends on the initial eccentricities and the planet mass. This result extend those of Chambers et al.(Icarus. 119,261-268) and Yoshinaga et al (1999, Icarus, 139, 328-335) where they found $log T= B \\Delta a +C$ at small $Delta a$. The unstable time has been connected with the Lyapunov time. These results are applied to the stability of observed extra-solar planet systems, especially that the observed a-e distribution can be explained by n-body interactions. POSTER: YES POSTER TITLE: Accretion of Heavy Elements to a Growing Giant Planet ABSTRACT: We investigate the efficiency of the planetesimal accretion to a protoplanet, after the core of the protoplanet is formed and it begins to accrete gas. We demonstrate a planetesimal gap will form soon near the protoplanet which may prevent further planetesimal accretion.The time scale for the gap opening and the width of the gap are derived analytically. We find the bombardments of planetesimals occur mainly on the late stage of the protoplanet gas accretion, and the mass range of individual planetesimals that could be effectively accreted to the protoplanet lies in the range of $10^{20}\\sim 10^{26}$ grams. The runaway type of gas accretion model like Bondi accretion with a growth time scale $10^5\\sim 10^6$ years is preferred for the protoplanet to get a more efficient and late time planetesimal accretion. We also find that due to the gas drag and protoplanet secular perturbations, the density of the planetesimal disk could be slightly increased outside the orbit of the protoplanet, which will enhance the subsequent formation of planet cores outside the orbit of the seed protoplanet. ===================================================== LAST NAME: Ferrándiz FIRST NAME: José M. BIRTH PLACE: Alicante BIRTH DATE: 12/8/1954 AFFILIATION: University of Alicante e-MAIL: jm.ferrandiz@ua.es ARRIVAL DATE: 10/9/2005 DEPARTURE: 18/9/2005 SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Navarro FIRST NAME: Juan F. BIRTH PLACE: Alicante BIRTH DATE: 28/11/1973 AFFILIATION: University of Alicante e-MAIL: jf.navarro@ua.es ARRIVAL DATE: 10/9/2005 DEPARTURE: 18/9/2005 SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Perov FIRST NAME: Nikolay BIRTH PLACE: Yaroslavl, Russian Federation BIRTH DATE: 19, December, 1950 AFFILIATION: Professor of State Pedagogical University, Astronomical Observatory e-MAIL: perov@yspu.yar.ru ARRIVAL DATE: 11 DEPARTURE: 16 SINGLE ROOM: NO DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: YES POSTER TITLE: Invariants in One Type of Perturbed Motion of Comets and Meteors ABSTRACT: Changes in semimajor axes and eccentricities of particles of meteoric showers for long intervals of time due to the effect of Pointing-Robertson are under consideration analytically tractable. The integrals of motion are used for identification of meteoric showers and comets. ===================================================== LAST NAME: El ABDALAOUI FIRST NAME: EL HOUCEIN BIRTH PLACE: Marocco BIRTH DATE: 01/01/1996 AFFILIATION: Laboratoire de mathèmatiques de Raphael Salam, Universitè de Rouen, France e-MAIL: ElHoucein.ElAbdalaoui@univ-rouen.fr ARRIVAL DATE: September 2005 DEPARTURE: 15 September 2005 SINGLE ROOM: Yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: EL ABDALAOUI FIRST NAME: EL HOUCEIN BIRTH PLACE: MOROCCO BIRTH DATE: 01/01/1966 AFFILIATION: Laboratoire de mathèmatiques de Raphael Salem, Universitè de Rouen, France e-MAIL: elhoucein.elabdalaoui@univ-rouen.fr ARRIVAL DATE: 10 September 2005 DEPARTURE: 15 September 2005 SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Nour-Eddine FIRST NAME: NAJID BIRTH PLACE: Casablanca Morocco BIRTH DATE: 26-01-56 AFFILIATION: University Hassan II Casablanca e-MAIL: najid.nour_eddine@caramail.com ARRIVAL DATE: ******* DEPARTURE: ******* SINGLE ROOM: **** DOUBLE ROOM: **** POSSIBLY SHARED WITH: ***** TALK: Yes TITLE: POTENTIAL OF A WIRE BENT INTO A CIRCULAR SHAPE ABSTRACT: Abstract: In this article, I develop the calculation of the potential generated by a homogeneous wire bent into a circular shape (Gianni P. 2000). In a second time we develop a new method of perturbation. It gives an expression of the potential in terms of R, the radius of the circle. The potential is expressed as a sum of the Newtonian and a small term. The former will be considered as a perturbation. We give the orbits of a test particle in accordance with the initial conditions. Precession of perihelia or chaotic cases are proved (Murray and Dermott . 1999). In an accurate way, we must use a juxtaposition of such circular wires, in order to built a two dimensional disc Key words: Potential-Legender Polynoms-Rings-Saturn. POSTER: No POSTER TITLE: ************* ABSTRACT: *************** ===================================================== LAST NAME: Rosaev FIRST NAME: Alexey BIRTH PLACE: Yaroslavl, Russia BIRTH DATE: 28.07.1959 AFFILIATION: FGUP NPC Nedra e-MAIL: rosaev@nedra.ru ARRIVAL DATE: 11.09.2005 DEPARTURE: 16.09.2005 SINGLE ROOM: No DOUBLE ROOM: Yes POSSIBLY SHARED WITH: Anybody TALK: Yes TITLE: THE PARAMETRIC INSTABILITY AT RESTRCITED N-BODY PROBLEM ABSTRACT: The planetary restricted three-body problem (RTBP) is considered. The primary mass M is much more than another masses mi, i=1..N, which revolve around M. The massless probe particle m0 moves on elliptic orbit, is perturbed by mi. Our target is - to study stability and instability in motion of m0 at resonance. It is well known, that equations of motion of restricted 3-body problem in rotating rectangular frame may be reduced to the second order differential equation with periodic coefficients (Hill’s equation). It gives the ability to estimate width and position of the unstable zones. Moreover, the dependence of the position of instable zones from orbital eccentricity of the probe particle is derived. It is evident, that overlapping of instability zones in strongly perturbed system can be a source of the chaotic behaviour. The main result of this work may be formulated in such form: There are not exist stable orbits with e=0 and i=0 in neighborhood of mean motion resonances (2n-1)/(2n+1). Positions and width of unstable zones depends from eccentricity. At high order of resonance, instable zones are overlapped. This fact can explain chaotic nature of according orbits. POSTER: Yes POSTER TITLE: A SEARCH FOR THE PERIODIC SOLUTIONS OF THE 2:1 RESONANCE RTBP BY NUMERIC INTEGRATION ABSTRACT: The 2:1 mean motion resonance orbit was integrated. Orbit of Jupiter was assumed circular. The start of first series of integration was from conjunction point at zero inclination and fixed eccentricity e=0.4 and different pericenter longitudes. The orbit with encounter at apocenter shows fast clockwise ===================================================== LAST NAME: NOYELLES FIRST NAME: Benoît BIRTH PLACE: LILLE (FRANCE) BIRTH DATE: 16th Nov 1978 AFFILIATION: IMCCE - Observatoire de Paris e-MAIL: Benoit.Noyelles@imcce.fr ARRIVAL DATE: 10th Sept. DEPARTURE: 16th Sept. SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: YES TITLE: Stochastic behaviour around the 3:7 inequality between Ganymede and Callisto ABSTRACT: The 3:7 inequality between J-3 Ganymede and J-4 Callisto, known as De Haerdtl\'s inequality, induces long period terms in the ephemerides of the Galilean satellites, but might have also been a source of stochatic behaviour in a recent past. This study describes the stochastic layers crossed by the system because of tidal effects and evaluates their influence on its actual state. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: VIENNE FIRST NAME: Alain BIRTH PLACE: Houdain (France) BIRTH DATE: 9th sep 1963 AFFILIATION: IMCCE - Observatoire de Paris e-MAIL: alain.vienne@imcce.fr ARRIVAL DATE: 11 sep DEPARTURE: 16 sep SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: Stochastic behaviour around the 3:7 inequality between Ganymede and Callisto ABSTRACT: (See Benoit Noyelles) POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: NOYELLES FIRST NAME: Benoît BIRTH PLACE: LILLE (FRANCE) BIRTH DATE: 16th Nov 1978 AFFILIATION: IMCCE - Observatoire de Paris e-MAIL: Benoit.Noyelles@imcce.fr ARRIVAL DATE: 11th Sept. DEPARTURE: 16th Sept. SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: YES TITLE: Stochastic behaviour around the 3:7 inequality between Ganymede and Callisto ABSTRACT: The 3:7 inequality between J-3 Ganymede and J-4 Callisto, known as De Haerdtl\'s inequality, induces long period terms in the ephemerides of the Galilean satellites, but might have also been a source of stochatic behaviour in a recent past. This study describes the stochastic layers crossed by the system because of tidal effects and evaluates their influence on its actual state. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Kuznetsov FIRST NAME: Eduard BIRTH PLACE: Russia BIRTH DATE: 03 Nov 1964 AFFILIATION: Astronomical Observatory of the Urals State University e-MAIL: Eduard.Kuznetsov@usu.ru ARRIVAL DATE: 11 Sep 2005 DEPARTURE: 17 Sep 2005 SINGLE ROOM: No DOUBLE ROOM: Yes POSSIBLY SHARED WITH: any TALK: Yes TITLE: K.V.Kholshevnikov, E.D.Kuznetsov \"Dynamical evolution of a weakly perturbed Two-Planetary System on a cosmogonic time-scale\" ABSTRACT: We consider orbital evolution of planetary systems similar to our Solar. In the present work we use Jacobian coordinates, construct the Hamiltonian expansions in the Poisson series in all elements for the planetary three-body problem with arbitrary values for planetary masses and mean semi-major axes its orbits. Further we construct the averaged Hamiltonian by the Hori~--- Deprit method with accuracy upto second order with respect to the small parameter, the generating function of the Lie transform, change of variables formulae, and right-hand sides of averaged equations. Resonant semi-major axes and estimations of the resonant zones width are obtained for the small parameter values varied from 0.001 to 0.1. The averaged equations are integrated numerically. Orbital evolution of the Sun~--- Jupiter~--- Saturn system and several of a weakly perturbed two-planetary systems are investigated at the time-scale 10 Gyr. This work was partly supported by the Leading Scientific School, Grant NSh-1078.2003.02. POSTER: Yes POSTER TITLE: E.D.Kuznetsov, G.T.Kaiser \"Stochastic dynamics of geosynchronous satellites\" ABSTRACT: The orbital evolution of geosynchronous satellites moving near separatrices separating of the rotation and libration motions regions and the libration motions with respect to the one and two stable points was investigated. We consider the phase plane \"longitude of subsatellite point - semi-major axis\". The separatrices can migrate due to the perturbations. Sizes of the migrate regions are minimal near libration points. Decrease of distance between separatrices and increase of the separatrix migrate region due to growth of an inclination lead to overlap the separatrix location regions. The estimations of the stochasticity zones width with respect to the initial semi-major axes values are obtained. The zones width grows at increase of the satellite\'s area to mass ratio and decreases with growth of the orbital inclination. The stochasticity zones corresponding various separatrices are separated from each other. This work was partly supported by the RFBR, Grant 03-02-16313. ===================================================== LAST NAME: BARUTELLO FIRST NAME: VIVINA BIRTH PLACE: TORINO BIRTH DATE: 12/11/1976 AFFILIATION: Università di Milano-Bicocca e-MAIL: vivina.barutello@unimib.it ARRIVAL DATE: 10/09/05 DEPARTURE: 17/09/05 SINGLE ROOM: DOUBLE ROOM: YES POSSIBLY SHARED WITH: Susanna Terracini TALK: YES TITLE: pERIODIC SOLUTIONS FOR THE N-BODY PROBLEM ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Baidin FIRST NAME: Alexey BIRTH PLACE: Arkhangelsk\'s region, Russian Federation BIRTH DATE: 26, November, 1980 AFFILIATION: Post-graduate Student, Department of Physics of State Pedagogical University e-MAIL: perov@yspu.yar.ru ARRIVAL DATE: 11 DEPARTURE: 16 SINGLE ROOM: NO DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: YES POSTER TITLE: Determination of Perturbed Orbits of Double Stars ABSTRACT: A method of determination of perturbations of pericenter longitude and ascending node longitude are under consideration. The obtained results are used for searching of third bodies (exoplanets)in double systems of stars. ===================================================== LAST NAME: Lopez - Garcia FIRST NAME: Francisco BIRTH PLACE: Argentine BIRTH DATE: 06/10/39 AFFILIATION: Professor e-MAIL: flgarcia@casleo.gov.ar ARRIVAL DATE: 09/10/05 DEPARTURE: 09/16/05 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: With my wife (Zulema Lopez Garcia) TALK: NO TITLE: ABSTRACT: POSTER: YES POSTER TITLE: Dynamical Behaviour of Centaurs Objects Between 23 and 26 AU ABSTRACT: We have analyzed the dynamical behaviour of objects located in a position 22 < a < 26 AU which corresponds to the mean motion resonances 3:2 and 2:3 with Neptune and Uranus respectively. Mostly of the studied objects migrant toward the external part of the Solar System, called Kuiper belt, a scattered disk in the a > 30 AU region. Some are ejected of the Solar System with e → 1. Of the test particles studied less than 10% migrant toward the inner part, in some cases becoming Earth and Mars crossing. This fact may be a source of near-Earth objects (NEOs), as asteroids in the Main Belt lying near the 3:1 resonance with Jupiter. Many objects make numerous close approaches to Jupiter and Saturn. Others clones, a few, can reach the region a ~ 500 au, e ~ 0.78, i ~ 15° (Sedna: a = 509 au, e = 0.851, i = 11.9). This behaviour of some clones occur when Neptune has a = 28 au. ===================================================== LAST NAME: Sándor FIRST NAME: Zsolt BIRTH PLACE: Tirgu-Mures BIRTH DATE: 21. 06. 1970 AFFILIATION: Department of Astronomy, Eötvös University, Budapest, Hungary e-MAIL: Zs.Sandor@astro.elte.hu ARRIVAL DATE: 11. 09. 2005 DEPARTURE: 16. 09. 2005 SINGLE ROOM: no DOUBLE ROOM: yes POSSIBLY SHARED WITH: Dr. Christos Efthymiopoulos TALK: yes TITLE: Determination of orbital parameters of exoplanets from transit fotometry by using dynamical constraints ABSTRACT: Space missions in the near future (for example COROT and KEPLER) devoted to discover Earth-like exoplanets will use the transit photometry as detection method. The transit of an unseen planet before the disc of the hosting star results in the periodic dimming of the star\'s light intensity. From the period, the duration, and the shape of the light curve of the transit the orbital parameters of the exoplanet can be estimated only within some error limits. In this paper we investigate the possibility of refining the orbital parameters of an unseen exoplanet discovered by transit photometry when other massive planets are present in the system. The presence of a giant exoplanet results in appearing dynamically unstable regions in the phase space. Thich means a dynamical constraint in the sense that only those orbital parameters will be selected, which originate ordered orbits. By using chaos-detection methods (RLI, FLI, SALI), orbital solutions, which result in chaotic orbits can be avoided. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: berretti FIRST NAME: alberto BIRTH PLACE: roma BIRTH DATE: 4 giugno 1957 AFFILIATION: dipartimento di matematica, universita\' di tor vergata, roma e-MAIL: berretti@mat.uniroma2.it ARRIVAL DATE: 11 sett. 2005 DEPARTURE: 16 sett. 2005 SINGLE ROOM: yes DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: yes TITLE: selection rules for periodic orbits of a driven damped quartic oscillator ABSTRACT: In this paper we investigate the conditions under which periodic solutions of the nonlinear oscillator x\'\' + x^3 = 0 persist when the dfferential equation is perturbed so as to become x\'\' + x^3 + eps x^3 cos t + gamma x\' = 0. We conjecture that for any periodic orbit, characterised by its frequency omega, there exists a threshold for the damping coefficient , above which the orbit disappears, and that this threshold is infinitesimal in the perturbation parameter, with integer order depending on the frequency omega. Some rigorous analytical results toward the proof of these conjectures are provided. Moreover the relative size and shape of the basins of attraction of the existing stable periodic orbits are investigated numerically, giving further support to the validity of the conjectures. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Canalias FIRST NAME: Elisabet BIRTH PLACE: Olot (Spain) BIRTH DATE: 21-12-1979 AFFILIATION: Universitat Politècnica de Catalunya e-MAIL: elisabet.canalias@upc.edu ARRIVAL DATE: 11-09-2005 DEPARTURE: 17-09-2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Estrella Olmedo TALK: YES TITLE: On the scattering map and homoclinic connections between Lyapunov orbits ABSTRACT: Homoclinic and heteroclinic connections between planar Lyapunov orbits of the Sun-Earth and Earth-Moon models can be found by using their hyperbolic invariant manifolds and Poincare section representations. These connections can be classified in bifurcation families according to the range of values of the associated Jacobi constant. In the formalism of invariant manifolds (as the aforementioned Jacobi constant changes) the foliation of all Lyapunov orbits is a Normally Hyperbolic Invariant Manifold. In this context, the homoclinic connections correspond to the so called Scattering map of this NHIM into itself. In this work, the Scattering map is studied as a possible way to formally describe the asymptotic connections arising from the natural dynamics of the Sun-Earth and Earth-Moon problems (in collaboration with Pau Roldan). POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Di Salvo FIRST NAME: Alessio BIRTH PLACE: Roma BIRTH DATE: 19/12/1974 AFFILIATION: postgraduate student, Università degli Studi di Roma La Sapienza e-MAIL: Alessio.DiSalvo@fastwebnet.it ARRIVAL DATE: 11/05/2005 DEPARTURE: 16/05/2005 (after the end of the conference) SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: YES TITLE: Preliminary analysis of space missions to the Libration Point L2: trajectory design and launch options ABSTRACT: This work is focused on the detection, computation and analysis of \"free\" transfer trajectories from typical parking orbits to quasi periodic orbits around L2. Launch alternatives and general constraints due to possible mission requirements have been also included. The CRTBP is the mathematical model used to describe the motion of a spacecraft, computed by integrating the non linearized equations of motion. A shooting method has been designed and developed to determine the DeltaV for the perigee maneuver. For a launch from Kourou, Ariane5 ES/ECA GTO and Soyuz GTO equivalent have been compared, considering DeltaV for the transfer maneuver, launch date, amplitudes of the final Lissajous orbit, transfer duration, variations of the declination and of the Sun–Vehicle–Earth angle, eclipse conditions, launcher performance and injection accuracy. This analysis highlights advantages and drawbacks of different parking orbits and launch options. Mission goals are anyway the key factors for the trade-off among orbit selection, launch alternatives and all the other constraints, fixed by the mission requirements POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: ROLDAN FIRST NAME: PABLO BIRTH PLACE: BARCELONA BIRTH DATE: 13/8/1975 AFFILIATION: UNIVERSITAT POLITECNICA DE CATALUNYA e-MAIL: PABLO.ROLDAN@UPC.ES ARRIVAL DATE: 11/9 DEPARTURE: 16/9 SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: YES TITLE: On the scattering map and homoclinic connections between Lyapunov orbits ABSTRACT: Homoclinic and heteroclinic connections between planar Lyapunov orbits of the Sun-Earth and Earth-Moon models can be found by using their hyperbolic invariant manifolds and Poincare section representations. These connections can be classified in bifurcation families according to the range of values of the associated Jacobi constant. In the formalism of invariant manifolds (as the aforementioned Jacobi constant changes) the foliation of all Lyapunov orbits is a Normally Hyperbolic Invariant Manifold. In this context, the homoclinic connections correspond to the so called Scattering map of this NHIM into itself. In this work, the Scattering map is studied as a possible way to formally describe the asymptotic connections arising from the natural dynamics of the Sun-Earth and Earth-Moon problems (in collaboration with Elisabet Canalias). POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Giorgilli FIRST NAME: Antonio BIRTH PLACE: Villasanta BIRTH DATE: 20-10-49 AFFILIATION: Universita\' di Milano Bicocca e-MAIL: antonio.giorgilli@unimib.it ARRIVAL DATE: 11-09-05 DEPARTURE: 16-09-05 SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Cors FIRST NAME: Josep M. BIRTH PLACE: Manresa, Catalonia. BIRTH DATE: 1/5/1965 AFFILIATION: UPC (Universitat Politècnica de Catalunya) e-MAIL: cors@eupm.upc.es ARRIVAL DATE: 11/9/2005 DEPARTURE: 17/9/2005 SINGLE ROOM: No DOUBLE ROOM: Yes POSSIBLY SHARED WITH: Jaume Soler (participant) TALK: Yes TITLE: Coorbital Periodic Orbits in the Three Body Problem ABSTRACT: We consider the dynamics of coorbital motion of two small moons about a large planet which have nearly circular orbits with almost equal radii. These moons avoid collision because they switch orbits during each close encounter. We approach the problem as a perturbation of decoupled Kepler problems. The perturbation is large but only in a small region in the phase space. We discuss the relationship required among the small quantities (radial separation, mass, and minimum angular separation) that admits coorbital motion like that observed for the moons of Saturn, Janus and Epimetheus. Persistence of the orbits is also given. POSTER: No POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Fasso` FIRST NAME: Francesco BIRTH PLACE: Milano BIRTH DATE: 07.10.1956 AFFILIATION: University of Padova e-MAIL: fasso@math.unipd.it ARRIVAL DATE: 11.09.2005 DEPARTURE: 16.09.2005 SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: YES TITLE: Long-term stability of L4 and L5 beyond Routh critical mass ABSTRACT: We study the global properties of the dynamics of the restricted three body problem near L4 and L5 for values of the mass ratio beyond Routh threshold, with special attention to the stability and regularity properties of motions nearby these (Lyapunov) unstable equilibria. Joint work with A. Giacobbe and M. Guzzo. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Efthymiopoulos FIRST NAME: Christos BIRTH PLACE: Athens BIRTH DATE: 24/1/1971 AFFILIATION: Research Center for Astronomy and Applied Mathematics, Academy of Athens e-MAIL: cefthim@cc.uoa.gr ARRIVAL DATE: 11/09/2005 DEPARTURE: 16/09/2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Zsolt Sandor TALK: YES TITLE: Computer-Assisted Nekhoroshev stability estimates for solar system dynamics ABSTRACT: This talk will review some recent progress, assisted by computer algebra, in understanding the patterns of accumulation of small divisors in the Birkhoff normal form and the way the latter affects the estimates of Nekhoroshev stability in nonlinear Hamiltonian dynamical systems. Examples are given with reference to the stability of Trojan objects in the neighborhood of the L4 and L5 stable equilibria. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: De Saedeleer FIRST NAME: Bernard BIRTH PLACE: Ixelles BIRTH DATE: 03/02/1970 AFFILIATION: FUNDP e-MAIL: bernard.desaedeleer@fundp.ac.be ARRIVAL DATE: 11/09/05 DEPARTURE: 16/09/05 SINGLE ROOM: DOUBLE ROOM: YES POSSIBLY SHARED WITH: D\'Hoedt Sandrine TALK: YES TITLE: Analytical Theory of Perturbations with third body effect of the Earth for a lunar artificial satellite ABSTRACT: We present here the main results of our analytical theory of an artificial satellite of the Moon. We use the Lie Transform as perturbation method for averaging the Hamiltonian of the problem, in canonical variables. Short period terms (linked to $l$, the mean anomaly) are eliminated first, and then the long period terms (linked to $g$ and $h$). The main perturbations are the synchronous rotation of the Moon (rate $n$), the triaxiality of the Moon ($C_{22} \\approx J_2/10$) and the major third body effect of the Earth (we use the lunar theory ELP2000 [Chapront, J. and Chapront-Touz\\\'e]). The solution is developed in powers of these small factors. We use our home-made Algebraic Manipulator, the MM (\"Moon\'s series Manipulator\"). The results are obtained in a closed form, without any series developments in eccentricity nor inclination. So the solution apply for a wide range of values, except for few isolated critical values. Numerical integrations are performed in order to validate our analytical theory. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Süli FIRST NAME: Áron BIRTH PLACE: Budapest BIRTH DATE: 1973 AFFILIATION: Eötvös Loránd University Dept. of Astronomy e-MAIL: a.suli@astro.elte.hu ARRIVAL DATE: 05/09/10 DEPARTURE: 05/09/16 SINGLE ROOM: NO DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: YES TITLE: A detailed comparison of the different chaos detection methods ABSTRACT: Preliminary results are presented on a systematic and detailed comparison of the different Chaos Detection Methods (CDM). The method of LCE, FLI, SALI, MEGNO, RLI and FSN are shortly introduced and applied both to mappings and to continuous Hamiltonian systems. The results of the different methods are compared and a detailed discussion is presented. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Kovács FIRST NAME: Tamás BIRTH PLACE: Mohács BIRTH DATE: 04.08.1979. AFFILIATION: Eötvös Lorand Univ. Dept. of Astronomy e-MAIL: t.kovacs@astro.elte.hu ARRIVAL DATE: 11.09.2005. DEPARTURE: 16.09.2005. SINGLE ROOM: no DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: yes POSTER TITLE: On the dependens of the first order solution on the Laplace-coefficients ABSTRACT: In celestial mechanics the fundamental task is to predict the long time evolution of planetary orbits. The secular evolution of the orbits was investigated first by Lagrange and Laplace in the framwork of the first order secular theory, the so called Laplace-Lagrange theory. In this study the Laplace-coefficients are calculated via different methods, and the corresponding solutions are compared to each other. They are also checked against to a numerical integration of the complete Solar System. These investigations help to choose the most accurate method. The long term evolution of the orbital elements depends on the Laplace-coefficients, the more accurate therefore the Laplace-coefficients are, the more reliable the corresponding solution is. ===================================================== LAST NAME: Dr. Hagel FIRST NAME: Johannes BIRTH PLACE: Graz BIRTH DATE: 30.5.1956 AFFILIATION: Institut für Psycho-Physik e-MAIL: ipp-koeln@netcologne.de ARRIVAL DATE: 11.9.2005 DEPARTURE: 16.9.2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: YES POSTER TITLE: Boundedness of solutions for dynamical systems depending on the initial conditions ABSTRACT: ABSTRACT: It is a well known fact that the boundedness properties of solutions to nonlinear differential equations which describe dynamical systems do depend on their initial conditions (positions and velocities). However, by application of even high order perturbation teory this property is usually not reflected by the analytical approximations to the solution. This is due to the fact that transitions to unbounded behaviour are topological changes of the solution geometry which are related to convergence breakdown of the associated series. In order to overcome this basic difficulty, the author developed a method which transforms at least certain classes of equations to an iterative system of linear differential equations containing the systems initial conditions explicitly in their coefficient function. Doing so we can in principle reduce the problem to a succession of linear stability analysis computations and we can expect to obtain information about the boundedness of some dynamical systems. In this work we shall apply the method to a cubic, explicitly time dependent second order differential equation and as a consequence of that to a simplified model of the Sitnikov problem. ===================================================== LAST NAME: Breiter FIRST NAME: Slawomir BIRTH PLACE: Poznan - Poland BIRTH DATE: 31.12.1963 AFFILIATION: Astronomical Observatory, A. Mickiewicz University, Poznan e-MAIL: breiter@amu.edu.pl ARRIVAL DATE: 11.09 DEPARTURE: 16.09 SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: YES TITLE: Critical Inclination in the Main Problem of a Massive Satellite ABSTRACT: Critical Inclination in the Main Problem of a Massive Satellite Authors: Slawomir Breiter and Antonio Elipe We extend the classical problem of the critical inclination in artificial satellite theory to the case when a satellite may have an arbitrary significant mass. If the planet\'s potential is restricted to the second zonal harmonic, according to the assumptions of the main problem of the satellite theory, two various phenomena can be observed: a critical inclination that asymptotically tends to the well known negligible mass limit, and a critical tilt that can be attributed to the effect of rotation of the gravity field harmonics to the invariant reference frame. Stability of this particular solution of the two rigid bodies problem is studied analytically and numerically. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: BARRABES FIRST NAME: ESTHER BIRTH PLACE: BARCELONA BIRTH DATE: 25/12/1967 AFFILIATION: UdG (Universitat de Girona) e-MAIL: barrabes@ima.udg.es ARRIVAL DATE: 11/09/2005 DEPARTURE: 17/09/2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Mercè Ollé (Participant) TALK: YES TITLE: Periodic solutions in the general 3-body problem coming from the elliptic restricted problem ABSTRACT: We consider solutions of the 3-body problem in which one mass is small (the mass parameter). The other two masses (the primaries) move approximately in elliptic keplerian motion and the small mass moves on a large near circular orbit in a plane perpendicular to that of the primaries. When the mass parameter tends to zero we obtain solutions of the elliptic restricted three body problem. (This is a joint work with J.Cors, C.Pinyol and J.Soler) POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Jopek FIRST NAME: Tadeusz BIRTH PLACE: Leszno, Poland BIRTH DATE: 1951.02.10 AFFILIATION: Astronomical Observatory of the AM University e-MAIL: jopek@amu.edu.pl ARRIVAL DATE: 11 Sept 2005 DEPARTURE: 16 Sept 2005 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: Searching for the parent of the Tunguska cosmic body ABSTRACT: In collaboration with Ch. Froeschle and R. Gonczi from Observatoire de Nice, France. POSTER: No POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Olmedo FIRST NAME: Estrella BIRTH PLACE: La Linea (Cádiz, Spain) BIRTH DATE: 10/09/1979 AFFILIATION: Universitat of Barcelona e-MAIL: estrella@maia.ub.es ARRIVAL DATE: 11/09/2005 DEPARTURE: 17/09/2005 SINGLE ROOM: DOUBLE ROOM: Yes POSSIBLY SHARED WITH: Elisabet Canalias TALK: Yes TITLE: Computing quasi-periodic motions for a particle in the Earth-Moon system: 2,3,4D-tori and their corresponding invariant manifolds (joint work with Angel Jorba) ABSTRACT: We are interested in the motion of a particle, such as a spacecraft or an asteroid, in the Earth-Moon System. The simplest model for this problem is the well known Restricted Three Body Problem (RTBP). Here we consider more realistic models that take into account the main perturbations coming from the Sun and the non-circular motion of Earth and Moon. These models are written as quasi-periodic time-dependent perturbations of the RTBP. In our case, depending on the number of effects considered, the perturbation can have 2, 3 or 4 basic frequencies. In the RTBP, there are five equilibrium that here will become tori of dimension 2, 3 or 4, depending on the number of basic frequencies of the perturbation. Our goal is to compute the tori substituting the collinear equilibrium $L_{1,2}$, as well as their invariant unstable and stable manifolds. We will also talk about other quasi-periodic solutions appearing from the centre directions of these tori. In that case the dimension of the tori increase in one or two units. Due to the strong instability of these points, we use a parallel shooting technique that has the collateral effect of increasing the dimension of the phase space up to 24. We represent these tori and the Floquet transformations by (truncated) Fourier series. Due to the huge amount of computer resources needed, we have modified a previous software of the authors --that was already parallelised and adapted for a Beowulf cluster-- to adapt it to the particularities of this problem. In the talk we will discuss some details of this computation and the results obtained. POSTER: No POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Venturelli FIRST NAME: Andrea BIRTH PLACE: Sassuolo (MO), Italy BIRTH DATE: 05 November 1971 AFFILIATION: Université d\'Avignon. e-MAIL: Andrea.Venturelli@univ-avignon.fr ARRIVAL DATE: 11/09/05 DEPARTURE: 16/09/05 SINGLE ROOM: Yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: Yes TITLE: Parabolic Solutions of the three-body problem asymptotic to a lagrangian configuration. ABSTRACT: Using variation methods, we show that given a configuration of three body in the plane, there exists a parabolic starting from that given configuration and asymptotic to a lagrangian one. Moreover, this solution has zero angular momentum. POSTER: No POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: DELEFLIE FIRST NAME: Florent BIRTH PLACE: Ste Catherine les Arras (France) BIRTH DATE: 10th June 1975 AFFILIATION: University of Namur, Belgium, and OCA/GEMINI e-MAIL: Florent.Deleflie@obs-azur.fr ARRIVAL DATE: 11/09/2005 DEPARTURE: 17/09/2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: 1) Stephane Valk or 2) Nicolas Rambaux (ACCOMPANYING) TALK: YES TITLE: Impact of the web of resonances on the long term evolution of Galileo-like satellites. ABSTRACT: Florent Deleflie, Stéphane Valk, Massimiliano Guzzo, Anne Lemaître We detect the structure of the web of resonances for the Galileo-like satellites in a model accounting for the non spherical shape of the Earth and the luni--solar perturbations. In particular, we study to what extent the choice of the new nominal semi-major axis of the constellation modifies the long period appearing in the orbital motion, because of a combination between periods involved in the motion of the Moon, the Sun, and the Earth. In particular, we analyse the impact on the long term evolution of the orbital elements, in view of studying the long term evolution of the semi-major axis and the eccentricity of Galileo-like orbits: is there some chaos in that 4-body system ? POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Farrés Basiana FIRST NAME: Ariadna BIRTH PLACE: Barcelona BIRTH DATE: 03/09/1981 AFFILIATION: Universitat de Barcelona e-MAIL: ari@maia.ub.es ARRIVAL DATE: 11 septembre DEPARTURE: 18 septembre SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Gemma Huguet TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Kuznetsov FIRST NAME: Eduard BIRTH PLACE: Russia BIRTH DATE: 03 Nov 1964 AFFILIATION: Astronomical Observatory of the Urals State University e-MAIL: Eduard.Kuznetsov@usu.ru ARRIVAL DATE: 11 Sep 2005 DEPARTURE: 17 Sep 2005 SINGLE ROOM: No DOUBLE ROOM: Yes POSSIBLY SHARED WITH: any TALK: Yes TITLE: K.V.Kholshevnikov, E.D.Kuznetsov \"Dynamical evolution of a weakly perturbed Two-Planetary System on a cosmogonic time-scale\" (revised) ABSTRACT: We consider orbital evolution of planetary systems similar to our Solar one. In the present work we use Jacobian coordinates, construct the Hamiltonian expansions in the Poisson series in all elements for the planetary three-body problem. Values of planetary masses and mean semi-major axes of their orbits may be arbitrary. Further we construct the averaged Hamiltonian by the Hori - Deprit method with accuracy upto second order with respect to the small parameter, the generating function of the Lie transform, change of variables formulae, and right-hand sides of averaged equations. Resonant semi-major axes and estimations of the resonant zones width are obtained for the small parameter values varying from 0.001 to 0.1. The averaged equations are integrated numerically. Orbital evolution of the Sun-Jupiter-Saturn system and several other weakly perturbed two-planetary systems are investigated at the time-scale 10 Gyr. This work was partly supported by the Leading Scientific School, Grant NSh-1078.2003.02. POSTER: Yes POSTER TITLE: E.D.Kuznetsov, G.T.Kaiser \"Stochastic dynamics of geosynchronous satellites\" ABSTRACT: The orbital evolution of geosynchronous satellites moving near separatrices separating of the rotation and libration motions regions and the libration motions with respect to the one and two stable points was investigated. We consider the phase plane \"longitude of subsatellite point - semi-major axis\". The separatrices can migrate due to the perturbations. Sizes of the migrate regions are minimal near libration points. Decrease of distance between separatrices and increase of the separatrix migrate region due to growth of an inclination lead to overlap the separatrix location regions. The estimations of the stochasticity zones width with respect to the initial semi-major axes values are obtained. The zones width grows at increase of the satellite\\\'s area to mass ratio and decreases with growth of the orbital inclination. The stochasticity zones corresponding various separatrices are separated from each other. This work was partly supported by the RFBR, Grant 03-02-16313. ===================================================== LAST NAME: Voyatzis FIRST NAME: George BIRTH PLACE: Greece BIRTH DATE: 20/5/1965 AFFILIATION: Dept. of Physics, Univ. of Thessaloniki, 54124, Greece e-MAIL: voyatzis@auth.gr ARRIVAL DATE: 11/9/2005 DEPARTURE: 17/9/2005 SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: YES TITLE: Symmetric and asymmetric librations of 3:1 resonant planetary systems. An application to the extrasolar system 55Cnc. ABSTRACT: We study the dynamics of 3:1 resonant motion for planetary systems with two planets based on the model of the general planar three body problem. The exact mean motion resonance corresponds to periodic motion (in a rotating frame) and we computed all the basic families of symmetric and asymmetric periodic orbits. Four symmetric families bifurcate from the family of circular orbits of the two planets and the asymmetric families bifurcate from the symmetric families at the points where the stability index becomes critical. There exist also asymmetric families that are independent of the above mentioned families. Resonant librating motion is found around stable periodic orbits. Therefore, the stable periodic orbits (symmetric or asymmetric) determine the possible stable configurations of the system even if the orbits of the two planets intersect. In the particular study, many periodic orbits are weakly unstable, but the Poincare sections indicate that these periodic orbits are also surrounded by invariant tori of regular motion and chaos is practically absent for low or moderate values of the eccentricity. An application is made for the extrasolar planetary system 55Cnc. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: SAHA FIRST NAME: LAL MOHAN BIRTH PLACE: TALPAHARI, INDIA BIRTH DATE: 23-06-1943 AFFILIATION: ZAKIR HUSAIN COLLEGE, DELHI UNIVERSITY e-MAIL: lms@iic.ac.in ARRIVAL DATE: 10-09-2005 DEPARTURE: 16-09-2005 SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: NIL TALK: YES TITLE: ON THE EFFECT OF POYNTING-ROBERTSON DRAG ON NONLINEAR ABSTRACT: Nonlinear stability of motion in the presence of Poynting-Robertson drag in a binary star system has been investigated within the framework of restricted three body problem. For different radiation parameters of binaries and varying initial conditions the transition from regular to chaotic motion of trajectories has been investigated using nonlinear forcasting method as used in nonlinear dynamics. Results are shown to compare well with those obtained using Poincare surface of sections. POSTER: NO POSTER TITLE: NOT APPLICABLE ABSTRACT: NOT APPLICABLE ===================================================== LAST NAME: Arona FIRST NAME: Lorenzo BIRTH PLACE: Voghera BIRTH DATE: 25-10-1978 AFFILIATION: Politecnico di Milano e-MAIL: lorarona@hotmail.com ARRIVAL DATE: 11-09-05 DEPARTURE: 16-09-05 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Erdi FIRST NAME: Balint BIRTH PLACE: Esztergom, Hungary BIRTH DATE: 1945.03.30 AFFILIATION: Department of Astronomy, Eotvos University, Budapest e-MAIL: B.Erdi@astro.elte.hu ARRIVAL DATE: 11.09.2005 DEPARTURE: 16.09.2005 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: Stability of Trojan planets in exoplanetary systems ABSTRACT: We investigate the stability of possible Trojan planets in exoplanetary systems. If a giant planet moves in the habitable zone of an exoplanetary system, the existence of terrestrial planets in the habitable zone is questionable. However, habitable terrestrial planets could exist around the stable Lagrangian points L4 or L5 of the giant planet. By using numerical methods we determine the size of the stability region around L4 and L5 depending on the mass and orbital eccentricity of the giant planet and the mass of the terrestrial planet. We discuss the features of the stability regions such as the ring-like structures coresponding to higher order resonances. As examples we study several exoplanetary systems, where the only known giant planet moves in the habitable zone. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Belló Mora FIRST NAME: Miguel BIRTH PLACE: Puertollano BIRTH DATE: 21-04-61 AFFILIATION: Deimos Space e-MAIL: miguel.bello@deimos-space.com ARRIVAL DATE: 00/00/00 DEPARTURE: 00/00/00 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: ABSTRACT: POSTER: N/A POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Masaki FIRST NAME: Yoshimitsu BIRTH PLACE: Japan BIRTH DATE: Sep. 1973 AFFILIATION: Geographical Survey Institute e-MAIL: ymasaki@gsi.go.jp ARRIVAL DATE: Sep.11 DEPARTURE: Sep.16 SINGLE ROOM: yes DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Post FIRST NAME: Marcus BIRTH PLACE: Herford (Germany) BIRTH DATE: 12.05.1979 AFFILIATION: University of Paderborn, Department of Mathematics e-MAIL: mpost@math.upb.de ARRIVAL DATE: 11 Sep 2005 DEPARTURE: 16 Sep 2005 SINGLE ROOM: yes DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: yes TITLE: On Target for Venus ABSTRACT: Recently, new techniques for the design of energy efficient trajectories for space missions have been proposed that are based on the circular restricted three body problem as the underlying mathematical model. These techniques exploit the structure of certain invariant sets and associated invariant manifolds in phase space in order to systematically construct energy efficient flight paths. We extend this model in order to account for a control force continuously applied on the spacecraft as realized by low thrust propulsion systems. We show how the techniques for the trajectory design can be suitably augmented. As an example we compute approximations to trajectories for a mission to Venus. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Giacobbe FIRST NAME: Andrea BIRTH PLACE: Venezia BIRTH DATE: 28/12/1970 AFFILIATION: Universita\' di Padova e-MAIL: giacobbe@math.unipd.it ARRIVAL DATE: 11/09/2005 DEPARTURE: 16/09/2005 SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: youssef FIRST NAME: manal BIRTH PLACE: Giza, Egypt BIRTH DATE: 30-9-64 AFFILIATION: Lecutrer in Astronomy Dept., Faculty of Science, Cairo university. e-MAIL: manal@frcu.eun.eg ARRIVAL DATE: 10 DEPARTURE: 17 SINGLE ROOM: DOUBLE ROOM: yes POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: yes POSTER TITLE: Three-dimensional periodic orbits about the triangular equilibrium points of the generalized restricted problem of three bodies ABSTRACT: In this papaer the generalized circular problem of three bodies has been considered. We have assumed that the infinitesimal mass be an oblate spheroid. The three-dimensional periodic solutions about the triangular equilibrium point are studied. Four-order approximation of the periodic solution has been obtained. The results are important to study te periodic orbits of axisymmetric cosmic laboratory about the trianular equilibrium points of Earth-Moon or Sun-Jupiter for example. ===================================================== LAST NAME: youssef FIRST NAME: manal BIRTH PLACE: Giza, Egypt BIRTH DATE: 30-9-64 AFFILIATION: Lecutrer in Astronomy Dept., Faculty of Science, Cairo university. e-MAIL: manal@frcu.eun.eg ARRIVAL DATE: 10 DEPARTURE: 17 SINGLE ROOM: DOUBLE ROOM: yes POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: yes POSTER TITLE: Three-dimensional periodic orbits about the triangular equilibrium points of the generalized restricted problem of three bodies ABSTRACT: In this papaer the generalized circular problem of three bodies has been considered. We have assumed that the infinitesimal mass be an oblate spheroid. The three-dimensional periodic solutions about the triangular equilibrium point are studied. Four-order approximation of the periodic solution has been obtained. The results are important to study te periodic orbits of axisymmetric cosmic laboratory about the trianular equilibrium points of Earth-Moon or Sun-Jupiter for example. ===================================================== LAST NAME: Smirnova FIRST NAME: Luybov BIRTH PLACE: Russia Yaroslavl BIRTH DATE: 19.07.81 AFFILIATION: Post-graduate student of Depatment of physics State Pedagogical university e-MAIL: LubaSM@yandex.ru ARRIVAL DATE: 11.09.05 DEPARTURE: 16.09.05 SINGLE ROOM: NO DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: YES POSTER TITLE: The Gould Belt and vector Laplasa ABSTRACT: The Gould Belt (named in honour of opened its in 1879 of american astronomer of Benjamin Àntorp Gould) was discovered as a result the statistical separation on the background of galactic disk of bright stars before 4 starry values, though as far back as 1847 on he indicated Hershel. The Gould belts can separation amongst the other stars of the Galaxy because system has an own dynamics. The System moves in a gravitational field of the Galaxy with U=a/r (a=GMG, G is gravitation constant and MG is a mass of the Galaxy). There is integral of the motion specific for each star and named by vector Laplasa. This vector is directed along semimajor axes from focus to perihelion and his value is ae. If Local system real exists as united integer, this vector must remain same for any star of the system. In this work investigate excerpt 347 stars of the catalogue HIPPARCOS located on distance 300kpc. For each star from excerpt determined a module of the vector and his galactic coordinates. ===================================================== LAST NAME: Vecchiato FIRST NAME: Stefania BIRTH PLACE: Roma BIRTH DATE: 04/07/1982 AFFILIATION: Università di Roma Tor Vergata e-MAIL: stefania.10@katamail.com ARRIVAL DATE: 11/09 DEPARTURE: 16/09 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Letizia Stefanelli TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Pitjeva FIRST NAME: Elena BIRTH PLACE: Gorky, Russia BIRTH DATE: 04.04.1950 AFFILIATION: Dr., senior staff researcher e-MAIL: evp@quasar.ipa.nw.ru ARRIVAL DATE: 11.09.2005 DEPARTURE: 18.09.2005 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: The asteroid impact on planets and mass estimations of asteroids and the main asteroid belt from ranging ABSTRACT: The significant impact of main belt asteroids on the inner planets and Kuiper belt objects on the position of the Sun was shown by numerical integration and should be taken into account when high-accuracy planetary ephemerides are constructed. From an analysis of motions of the major planets some physical parameters of the asteroids were obtained by processing of precise measurements of ranging (1961-2003). The masses of the 6 asteroids were determined individually, masses of the most relevant 296 asteroids were derived from their latest published diameters making use of the corresponding densities. The total contribution of all remaining small asteroids was modeled as an acceleration caused by a solid ring. As a sequence the total mass of the main asteroid belt was obtained: M=(15+-1)*10E-10 mass of Sun. An derived expression for estimating the total number of minor planets in any unit interval of absolute magnitude H was compared with the observed distributions of the 233001 asteroids. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Carruba FIRST NAME: Valerio BIRTH PLACE: Rome, Italy BIRTH DATE: 02/07/1970 AFFILIATION: IAG-USP e-MAIL: valerio@astro.iag.usp.br ARRIVAL DATE: 11/09/2005 DEPARTURE: 16/09/2005 SINGLE ROOM: DOUBLE ROOM: Yes POSSIBLY SHARED WITH: Andrea Goulart Mendes Carruba (ACCOMPANYING) TALK: Yes TITLE: On the V-type asteroids outside the Vesta family: dynamical evolution via nonlinear secular resonances and the Yarkovsky effect: the cases of 809 Lundia,956 Elisa, and 6406 1992 MJ ABSTRACT: Among the largest objects in the main belt, asteroid 4 Vesta has been known as the unique to show a basaltic crust. Vesta is the largest member of the Vesta family, that is supposed to originate from a large cratering event about 1 Byr ago (Marzari et al. 1996, Thomas et al. 1997). Most members of the dynamical Vesta family show a V-type spectra, characterized by a moderately steep red slope shortwards of 0.7 micron and a deep absorption band long-wards of 0.75 micron. Due to their characteristic spectrum, V-type asteroids are easily distinguished. Before the discovery of 1459 Magnya (Lazzaro et al. 2000) and of several V-type NEA (Cruikshank et al., 1991, Wisniewski et al. 1991, Xu et al. 1995), all the known V-type asteroids were member of the Vesta family. Recently two V-type asteroids (809 Lundia and 956 Elisa, Florczak et al., 2002) have been discovered near the Flora family, well outside the limits of the Vesta family. We currently know 28 V-type asteroids outside the family, in the inner asteroid belt. In this work we investigate the possibility that these objects are family members that dynamically migrated to their current positions. Previous studies (Roig et al., in preparation) showed that the most believed mechanisms of dynamical mobility, --chaotic diffusion via three-body mean motion resonances, nonlinear secular resonances and the Yarkovksy non-gravitational force--, could not account for the observed orbital distribution of the V-type asteroids over the length of the integration (500 Myr), when considered separately. Evolution via secular resonances happens on timescales that are longer than the age of the family, while the Yarkovsky effect, which mostly modify the asteroids semi-major axes, could not produce the observed values of proper eccentricity and inclination of the 28 V-type asteroids. Here we investigate another possible scenario: evolution in nonlinear secular resonances due to Yarkovsky effect. Our simulations show that members of the Vesta dynamical family captured in three-body and secular resonances may drift until they reach the 2(g-g6)+s-s6 (z2, in the notation of Milani and Knezevic, 1993) secular resonance, where they are temporary captured for timescales of 1 Byr or more. This two-step mechanism could explain the current resonant orbits of 809 Lundia, 956 Elisa, and 6406 1992 MJ. We believe other V-type asteroids could have followed the same path, and currently be inside the z2 resonance. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: ferrario FIRST NAME: davide l. BIRTH PLACE: monza (mi) BIRTH DATE: 04/08/1969 AFFILIATION: dipartimento di matematica e applicazioni - università di milano-bicocca e-MAIL: davide.ferrario@unimib.it ARRIVAL DATE: 10/sep DEPARTURE: 16/sep SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Huguet FIRST NAME: Gemma BIRTH PLACE: Sant Marti de Riucorb (Lleida) BIRTH DATE: 23/09/80 AFFILIATION: Phd student e-MAIL: gemma.huguet@upc.edu ARRIVAL DATE: 11/09/2005 DEPARTURE: 16/09/2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Ariadna Farres TALK: NO TITLE: ABSTRACT: POSTER: YES POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Soler FIRST NAME: Jaume BIRTH PLACE: Barcelona (Spain) BIRTH DATE: 25/07/54 AFFILIATION: Universitat de Girona e-MAIL: jaume.soler@udg.es ARRIVAL DATE: 10/09/05 DEPARTURE: 16/09/05 SINGLE ROOM: no DOUBLE ROOM: yes POSSIBLY SHARED WITH: Josep M. Cors TALK: yes TITLE: Periodic Solutions in the Elliptic Restricted Three-Body Problem ABSTRACT: A discrete family of symmetric periodic solutions in the restricted elliptic three-body problem is shown to exist in the case of arbitrary masses of the primaries and arbitrary eccentricity of their orbit. The infinitesimal body moves on a nearly circular orbit of very large radius with a period multiple of that of the primaries. Averaging and and an implicit function theorem of Arenstorf are the main tools in the proof of the result. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Vilhena de Moraes FIRST NAME: Rodolpho BIRTH PLACE: BRAZIL BIRTH DATE: juin/05/40 AFFILIATION: FEG/UNESP e-MAIL: rodolpho@feg.unesp.br ARRIVAL DATE: 11-SEPT DEPARTURE: 16-SEPT SINGLE ROOM: DOUBLE ROOM: YES POSSIBLY SHARED WITH: ACCOMPANYING TALK: YES TITLE: Attitude Equilibrium of a Satellite Subject to Gravity Gradient Torque ABSTRACT: The stability analysis of the rotational motion of an artificial satellite under the influence of external torques can be mandatory for the success of some space missions. In this paper the stability analysis is performed using Hamiltonian formalism and a normal form for the Hamiltonian. Using Lie-Hori theory the Hamiltonian is normalized up to order four, in the neighborhoods of the equilibrium points. The equations considered for the rotational motion includes the gravity gradient torque and are described by the Andoyer variables. The equilibrium points and stability regions are established. POSTER: Yes POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: YANGUAS FIRST NAME: PATRICIA BIRTH PLACE: SPAIN BIRTH DATE: 8-8-1969 AFFILIATION: UNIVERSIDAD PUBLICA DE NAVARRA e-MAIL: YANGUAS@UNAVARRA.ES ARRIVAL DATE: 10-9-2005 DEPARTURE: 17-9-2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: JESUS F. PALACIAN TALK: YES TITLE: The spatial elliptic restricted three-body problem: periodic orbits ABSTRACT: Using a combination of analytical and numerical techniques we calculate new families of periodic orbits of the spatial elliptic restricted three-body problem. The initial conditions to numerically compute the orbits are given in an analytical way. After doubly averaging the Hamiltonian over the time and the mean anomaly we calculate its relative equilibria and study their linear and Lyapunov stability. This is used, not only to reconstruct invariant manifolds in the original system, but also to determine six families of periodic orbits with large semimajor axes having any eccentricity. Four families lie on a plane perpendicular to the plane of the primaries, two of them being stable and the other two unstable. The other two families are stable families of closed orbits coplanar with the primaries. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: PALACIAN FIRST NAME: JESUS F. BIRTH PLACE: SPAIN BIRTH DATE: 1-12-1965 AFFILIATION: UNIVERSIDAD PUBLICA DE NAVARRA e-MAIL: PALACIAN@UNAVARRA.ES ARRIVAL DATE: 10-9-2005 DEPARTURE: 17-9-2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: PATRICIA YANGUAS TALK: YES TITLE: The spatial elliptic restricted three-body problem: periodic orbits ABSTRACT: Using a combination of analytical and numerical techniques we calculate new families of periodic orbits of the spatial elliptic restricted three-body problem. The initial conditions to numerically compute the orbits are given in an analytical way. After doubly averaging the Hamiltonian over the time and the mean anomaly we calculate its relative equilibria and study their linear and Lyapunov stability. This is used, not only to reconstruct invariant manifolds in the original system, but also to determine six families of periodic orbits with large semimajor axes having any eccentricity. Four families lie on a plane perpendicular to the plane of the primaries, two of them being stable and the other two unstable. The other two families are stable families of closed orbits coplanar with the primaries. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Stefanelli FIRST NAME: Letizia BIRTH PLACE: Roma BIRTH DATE: 02/05/1982 AFFILIATION: Università di Roma Tor Vergata e-MAIL: stefanelliletizia@libero.it ARRIVAL DATE: 11/09/2005 DEPARTURE: 16/09/2005 SINGLE ROOM: no DOUBLE ROOM: yes POSSIBLY SHARED WITH: Stefania Vecchiato TALK: no TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Féjoz FIRST NAME: Jacques BIRTH PLACE: Lyon, France BIRTH DATE: 04/05/1973 AFFILIATION: Université P. & M. Curie e-MAIL: fejoz@math.jussieu.fr ARRIVAL DATE: 11/09/2005 DEPARTURE: 16/09/2005 SINGLE ROOM: DOUBLE ROOM: YES POSSIBLY SHARED WITH: Andrea Venturelli (?) TALK: Yes TITLE: About Arnold theorem ABSTRACT: Already given POSTER: No POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: D\'Hoedt FIRST NAME: Sandrine BIRTH PLACE: Charleroi (Belgium) BIRTH DATE: 20/04/1977 AFFILIATION: University of Namur (Belgium) e-MAIL: sandrine.dhoedt@fundp.ac.be ARRIVAL DATE: 11/09/2005 DEPARTURE: 16/09/2005 SINGLE ROOM: DOUBLE ROOM: Yes POSSIBLY SHARED WITH: Bernard De Saedeleer TALK: Yes TITLE: Mercury\'s Rotation : The four equilibria of the Hamiltonian model. (S. D\'Hoedt and N. Rambaux) ABSTRACT: Mercury is in a 3:2 spin-orbit resonance. The model presented here is limited to the second order in harmonics and Mercury is considered as a rigid body. In this framework, using a Hamiltonian formalism, four equilibria are computed from the differential Hamiltonian equations, and, thanks to the calculation of the corresponding eigen values, their stability is analyzed. In this simplified model, three of the 4 equilibria are degenerate, and the fourth one (corresponding to the present state of mercury) is stable. We show that this degenerescence is also present in the numerical results obtained by the software SONYR, with the same basic hypotheses. This degenerate status disappears with the introduction of the orbit precession, which explains its absence in the spin-orbit resonant motion of the Moon, for example. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: HOWARD FIRST NAME: JAMES BIRTH PLACE: USA BIRTH DATE: 7 June 1937 AFFILIATION: LASP, Univ. of Colorado at Boulder e-MAIL: jhoward@colorado.edu ARRIVAL DATE: 11 Sept 2005 DEPARTURE: 17 Sept 2005 SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: YES TITLE: ABSTRACT: Topology and Ergodicity in Planetary Dust Grain Dynamics J. E. Howard, M. Horanyi and L. Esposito Laboratory for Atmospheric and Space Physics University of Colorado, Boulder CO 80309 USA Charged dust grains orbiting Saturn are subject to the simultaneous influence of several different forces, including planetary gravitational and electromagnetic forces, plasma drag, and solar radiation pressure. In addition, sputtering producted by the erosive magnetospheric plasma leads to a significant diminution of submicron grain radii in a matter of decades. As it shrinks, a grain becomes more responsive to the electromagnetic forces, while the topology of the confining effective potential undergoes qualitative changes. At the same time the motion becomes more chaotic and therefore increasingly ergodic. The synergism of topology and ergodicity can lead to significant particle loss to the planet or to interplanetary space, while more regular orbits can remain trapped by local invariants. In addition, the symmetry-breaking effects of radiation pressure can enhance chaos, while planetary oblateness (J_2) can contribute to orbital ergodicity. The results are applied to the CDA experiment on the Cassini Spacecraft now orbiting Saturn. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Libert FIRST NAME: Anne-Sophie BIRTH PLACE: Brussels BIRTH DATE: 13/07/1982 AFFILIATION: University of Namur (FUNDP) e-MAIL: anne-sophie.libert@fundp.ac.be ARRIVAL DATE: 11/09/2005 DEPARTURE: 16/09/2005 SINGLE ROOM: yes DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: yes TITLE: Analytical Study of the (Exo)planetary Three Body Problem ABSTRACT: Exoplanetary systems are quite different from our own planetary system and classical Laplace-Lagrange linear perturbation theory is very limited. We analyze the secular interactions of two coplanar non-resonant planets with a high order expansion of the perturbative potential in powers of eccentricities . We show that this approach models correctly most of exosystems discovered so far. Particular attention is given to apsidal configuration, libration or circulation, oscillation amplitude of the angular difference of the apsidal lines... POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Valk FIRST NAME: Stéphane BIRTH PLACE: Namur (Belgium) BIRTH DATE: 13/05/1979 AFFILIATION: University of Namur, Belgium e-MAIL: stephane.valk@fundp.ac.be ARRIVAL DATE: 11/09/2005 DEPARTURE: 16/09/200517/09/2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Florent Deleflie (ACCOMPANYING) TALK: NO TITLE: ABSTRACT: POSTER: YES POSTER TITLE: Is the theory of mean orbital motion convenient to compute orbits of earth space debris ? ABSTRACT: Most of studies of orbits of clouds of space debris are based on statistical methods, to deduce from the trajectories the main characteristics of the motion, in particular over large time scales. The paper we propose here should be the first step to compute explicitly the long time evolution of orbits of a set of numerous space debris (10,000 typically) We propose, hence, to study if the theory of mean orbital motion, implemented in the CODIOR software, is adapted, or not, to such a goal. In particular, we will analyse, for LEO & MEO orbits, the impact of each term appearing in the equations of motion, deduced from analytical transformation. As a result, we will quantify and test the cpu load to compute simultaneously a wide range of trajectories. ===================================================== LAST NAME: Gabern FIRST NAME: Frederic BIRTH PLACE: Barcelona BIRTH DATE: 05-XII-1972 AFFILIATION: Universitat de Barcelona e-MAIL: gabern@maia.ub.es ARRIVAL DATE: 11-IX DEPARTURE: 16-IX SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: YES TITLE: Binary Asteroids Observation Orbits from a Global Dynamical Picture ABSTRACT: We study spacecraft motion near a binary asteroid. We model the system assuming that one of the asteroids is a rigid body (ellipsoid) and the other a sphere [2]. In particular, we are interested in finding periodic and quasi-periodic orbits for the spacecraft near the asteroid pair suitable to perform observations and measurements. First, using reduction theory [1], we study the full two body problem (gravitational interaction between the ellipsoid and the sphere) and use the energy--momentum method [3] to prove nonlinear stability of certain relative equilibria. This study allows us to construct the restricted full three body problem (RF3BP) for the spacecraft motion around the binary, assuming that the asteroid pair is in relative equilibrium. Then, we compute the modified Lagrangian fixed points and study their spectral stability. The fixed points of the restricted three body problem are modified in the RF3BP because one of the primaries is a rigid body and not a point mass. Here, a systematic study depending on the parameters of the problem is performed. Hence, we are interested in understanding the rigid body effects on the Lagrangian stability regions. Finally, using the frequency analysis method, we study the global dynamics near these modified Lagrangian points. From this global picture, we are able to identify (almost) invariant tori in the stability region near the modified Lagrangian points. Quasi-periodic trajectories on these invariant tori are very convenient to ``park\'\' the spacecraft on them, while the spacecraft is observing the asteroid pair. [1] J.E. Marsden and T.S. Ratiu, Introduction to mechanics and symmetry, volume 17 of Texts in Applied Mathematics. Springer-Verlag, New York, second edition, 1999. [2] D.J. Scheeres and J. Bellerose, The Restricted Hill Full 4-Body Problem: Application to spacecraft motion about binary asteroids. Dynamical Systems: An International Journal, 20(1):23--44, 2005. [3] J.C. Simo, D.Lewis, and J.E. Marsden, Stability of relative equilibria. I. The reduced energy-momentum method. Arch. Rational Mech. Anal., 115(1):15--59, 1991. (Joint work with W.S. Koon, J.E. Marsden and D.J. Scheeres) POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Vigueras FIRST NAME: Antonio BIRTH PLACE: Archena (Murcia), Spain BIRTH DATE: 07-11-1952 AFFILIATION: Universidad Politécnica de Cartagena e-MAIL: antonio.vigueras@upct.es ARRIVAL DATE: 10-09-2005 DEPARTURE: 17-09-2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Antonio Vigueras (Accompanying) TALK: YES TITLE: Relative equilibria for a gyrostat in the order k approximate dynamics of the three-body problem ABSTRACT: We consider the non-canonical Hamiltonian dynamics of a gyrostat in the three-body problem. As in Mondéjar et al. (2001), we obtain the equations of the reduced dynamics, then we give necessary and sufficient conditions for existence of relative equilibria type Euler, Lagrange and other (that we call “planar” rotations) in different approximations of the potential function. When the gyrostat is an axis-symmetric homogeneous ball (oblate or elongated), has a plane of symmetry and the gyrostatic momentum is constant, several families of relative equilibria of the previously mentioned types are obtained. In particular, for the first order approximation dynamics a complete study of the bifurcations of these relative equilibria is made. In this way, we generalise the classical results for the three-body problem and others (in which one of them is a rigid body or gyrostat) due to Fanny and Badoui (1998) and Mondéjar et al. (2001). POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Vigueras FIRST NAME: Antonio BIRTH PLACE: Archena (Murcia), Spain BIRTH DATE: 07-11-1952 AFFILIATION: Universidad Politecnica de Cartagena e-MAIL: antonio.vigueras@upct.es ARRIVAL DATE: 10-09-2005 DEPARTURE: 17-09-2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Adoracion Rodriguez (Accompanying) TALK: YES TITLE: Relative equilibria for a gyrostat in the order k approximate dynamics of the three-body problem ABSTRACT: We consider the non-canonical Hamiltonian dynamics of a gyrostat in the three-body problem. As in Mondejar et al. (2001), we obtain the equations of the reduced dynamics, then we give necessary and sufficient conditions for existence of relative equilibria type Euler, Lagrange and other (that we call \"planar\" rotations) in different approximations of the potential function. When the gyrostat is an axis-symmetric homogeneous ball (oblate or elongated), has a plane of symmetry and the gyrostatic momentum is constant, several families of relative equilibria of the previously mentioned types are obtained. In particular, for the first order approximation dynamics a complete study of the bifurcations of these relative equilibria is made. In this way, we generalise the classical results for the three-body problem and others (in which one of them is a rigid body or gyrostat) due to Fanny and Badoui (1998) and Mondejar et al. (2001). POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Di Lizia FIRST NAME: Pierluigi BIRTH PLACE: Chieti BIRTH DATE: 24/08/1978 AFFILIATION: PhD candidate, Dipartimento di Ingegneria Aerospaziale, Politecnico di Milano e-MAIL: dilizia@aero.polimi.it ARRIVAL DATE: 11/09/2005 DEPARTURE: 16/09/2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Paolo De Pascale TALK: YES TITLE: ON THE USE OF INTERVAL ARITHMETIC FOR THE PROPAGATION OF UNCERTAINTIES IN ORBITAL DYNAMICS ABSTRACT: In 1962 Moore formalized the theory of Interval Analysis, in which real numbers are substituted by intervals of real numbers, in order to allow a direct error control along the computation process. From that moment on, numerous applications of Interval Analysis appeared in several fields and opened the way to a different treatment of uncertainties in space related problems such as: numerical errors in the integration of n-body dynamics, uncertainties in orbit determination, unmodeled parameters or dynamical forces, etc… In this paper, the possibility of using interval arithmetic in common spaceflight mechanics problems has been assessed through a comparative analysis of interval integration techniques that might tackle these problems. Those techniques have been applied to the long term validated integration both of simple and perturbed motion of NEOs and compared to the application of interval arithmetic to the analytical solution available in terms of Lagrange coefficients. Then uncertainties both on initial conditions and on model parameters have been expressed in interval form and propagated through the above mentioned interval techniques in order to obtain an exact enclosure of final conditions. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Burov FIRST NAME: Alexander BIRTH PLACE: Moscow BIRTH DATE: 07.02.1958 AFFILIATION: Dorodnicyn Computing Center of the Russian Academy of Sciences e-MAIL: aburov@ccas.ru ARRIVAL DATE: 11.09.2005 DEPARTURE: 16.09.2005 SINGLE ROOM: no DOUBLE ROOM: yes POSSIBLY SHARED WITH: Burova Tatiana accomopanying TALK: yes TITLE: Restricted problems in Rigid Body Dynamics ABSTRACT: The restricted n-bodies problem as well as as the restricted n-vortices problem are well-known in mechanics. The applicability of the concept of \"restrictness\" to the problems of rigid body dynamics is demonstrated. The developed approach is applied to dynamics of heavy rigid bodies, satellites and bodies moving in an ideal fluid. POSTER: yes POSTER TITLE: Dynamics of satellites with attached massive points ABSTRACT: The attitude dynamics, reorientation and stbilisation of satellites with the use of the attached massive points attached by tethers is discussed. ===================================================== LAST NAME: Prokopenya FIRST NAME: Alexander BIRTH PLACE: Republic of Belarus BIRTH DATE: July 21, 1960 AFFILIATION: Brest State Technical University e-MAIL: prokopenya@brest.by ARRIVAL DATE: Sep. 11 DEPARTURE: Sep. 16 SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: YES TITLE: New Homographic Solutions in the Newtonian Many-Body Problem ABSTRACT: It is proved the existence of a general class of the homographic solutions in the Newtonian many-body problem. In the barycentric inertial frame of reference these solutions determine similar closed orbits of the bodies being the conic sections. But in a pulsating, non-uniformly rotating coordinate system they are corresponded to the equilibrium positions of the bodies which must form central configurations. We have obtained the equations giving the necessary and sufficient conditions of the solutions existence. The obtained equations are essentially nonlinear and can be solved only umerically. Using the system Mathematica, we have analyzed these equations for different numbers of the bodies. In the case of four interacting bodies, for example, we have shown that there exist central configurations in the form of a quadrangle if the bodies have different masses. If two bodies have equal masses the central configurations exist in the form of isosceles triangle with the fourth body being on the axis of symmetry of the triangle. There also exist central configurations when the bodies are at the vertices of concentric regular polygons, the bodies of equal masses being on the vertices of each polygon. The stability of the obtained homographic solutions is studied. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Armellin FIRST NAME: Roberto BIRTH PLACE: Messina BIRTH DATE: 23/03/1978 AFFILIATION: Politecnico di Milano e-MAIL: armellin@aero.polimi.it ARRIVAL DATE: 10 DEPARTURE: 16 SINGLE ROOM: no DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: yes TITLE: AEROGRAVITY ASSIST MANEUVRE FOR INTERPLANETARY MISSIONS: CONTROLLED DYNAMICS MODELLING AND OPTIMIZATION ABSTRACT: The aero-gravity assist manoeuvre is proposed as a method to improve the efficiency of the gravity assist. During this kind of manoeuvre the angular deviation of the velocity vector can be definitely increased thanks to the interaction with the planetary atmosphere. Even though the drag reduces the spacecraft velocity, the overall Äv gain could be remarkable whenever a high lift to drag vehicle is supposed to fly. Earlier studies show simplified approach according both to the dynamics modelling and the atmospheric trajectory constraints, as a planar motion together with a circular atmospheric path are imposed. In this paper a more realistic model is proposed, the planar motion constraint has been dropped and more refined estimate of the overall effect of the maneuver has been carried out. Some relevant aspects related to the multidisciplinary design has been considered like heat and structural loads bounding. Comparisons between in and out of plane manoeuvring have been performed by controlling either the angle of attack or the bank angle respectively. The optimal control problem has been solved by selecting a direct method approach. The dynamics has been transcribed into a set of nonlinear constraints and the arising Non Linear Programming problem has been solved with a SQP optimizer. To gain global optimum convergence the initial guess has been supplied by solving the same problem with a multi-objective approach supported by a direct shooting technique and a Genetic optimizer. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Szenkovits FIRST NAME: Ferenc BIRTH PLACE: Târgu-Mureº, Romania BIRTH DATE: 07.06.1959 AFFILIATION: Babeº-Bolyai University, Cluj-Napoca, Romania e-MAIL: fszenko@math.ubbcluj.ro ARRIVAL DATE: 11 sept. DEPARTURE: 16 sept. SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: TALK: YES TITLE: Hill stability in the elliptic restricted three-body problem ABSTRACT: We use a three dimensional generalization of Szebehely’s invariant relation obtained in the planar case of the elliptic restricted three-body problem to establish more accurate criteria of the Hill stability. By using these criteria, the stability of the natural satellites of our planetary system and of possible extra solar satellites is studied. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Armellin FIRST NAME: Roberto BIRTH PLACE: Messina BIRTH DATE: 23/03/1978 AFFILIATION: Politecnico di Milano e-MAIL: armellin@aero.polimi.it ARRIVAL DATE: 10 DEPARTURE: 16 SINGLE ROOM: no DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: yes TITLE: \" Aerogravity Assist Maneuvre for Interplanetary Missions: Controlled Dynamics Modeling and Optimization\" R. Armellin, M. Lavagna and A. Ercoli Finzi ABSTRACT: The aero-gravity assist manoeuvre is proposed as a method to improve the efficiency of the gravity assist. During this kind of manoeuvre the angular deviation of the velocity vector can be definitely increased thanks to the interaction with the planetary atmosphere. Even though the drag reduces the spacecraft velocity, the overall Äv gain could be remarkable whenever a high lift to drag vehicle is supposed to fly. Earlier studies show simplified approach according both to the dynamics modelling and the atmospheric trajectory constraints, as a planar motion together with a circular atmospheric path are imposed. In this paper a more realistic model is proposed, the planar motion constraint has been dropped and more refined estimate of the overall effect of the maneuver has been carried out. Some relevant aspects related to the multidisciplinary design has been considered like heat and structural loads bounding. Comparisons between in and out of plane manoeuvring have been performed by controlling either the angle of attack or the bank angle respectively. The optimal control problem has been solved by selecting a direct method approach. The dynamics has been transcribed into a set of nonlinear constraints and the arising Non Linear Programming problem has been solved with a SQP optimizer. To gain global optimum convergence the initial guess has been supplied by solving the same problem with a multi-objective approach supported by a direct shooting technique and a Genetic optimizer. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Japenga FIRST NAME: Sonja BIRTH PLACE: Dordrecht BIRTH DATE: 16-12-1969 AFFILIATION: Springer e-MAIL: Sonja.Japenga@springer-sbm.com ARRIVAL DATE: 10-9-2005 DEPARTURE: 16-9-2005 SINGLE ROOM: yes DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: De Pascale FIRST NAME: Paolo BIRTH PLACE: Roma BIRTH DATE: 13-07-1977 AFFILIATION: CISAS, University of Padova e-MAIL: depascale@pd.astro.it ARRIVAL DATE: 11-09 DEPARTURE: 16-09 SINGLE ROOM: no DOUBLE ROOM: YES POSSIBLY SHARED WITH: Pierluigi Di Lizia TALK: YES TITLE: A Dynamic Programming Based Algorithm for the Design of Low-Thrust Trajectories ABSTRACT: In this work a novel approach to the design of low-thrust transfers, based on dynamic programming, is presented. The optimal control problem associated to low-thrust trajectories is solved through a backward stage-wise local solution of the Hamilton-Jacobi-Bellman equation. The whole trajectory, is decomposed into a sequence of single stage problems of small dimensions, which are iteratively solved backward in time yielding the optimal control profile. This leads to a quadratic convergent algorithm whose computational cost grows linearly with the number of stages. This approach is more robust than traditional indirect methods and, for a high number of stages, more efficient than direct approaches. Moreover the stage wise solution of the problem allows, at each optimization step, an adjustment of the discretization grid through a variable step integration scheme. This property is particularly appealing in the treatment of variable scale highly non linear dynamics. Some results on the design of complex trajectories with multi-body dynamics and multiple spiralling orbits, commonly difficult for traditional methods, are presented. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Fantino FIRST NAME: Elena BIRTH PLACE: Venezia (Italy) BIRTH DATE: 12/10/1970 AFFILIATION: Dipartimento di Astronomia - Università di Padova e-MAIL: fantino@pd.astro.it ARRIVAL DATE: 11/09/2005 DEPARTURE: 16/09/2005 SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: YES TITLE: Low-energy transfer orbits in the elliptic restricted Three-Body Problem ABSTRACT: Casotto, S., Fantino E., Alessi E. M. The hyperbolic invariant manifolds associated with periodic orbits about libration points have proven to be a key ingredient in low-energy trajectory design and transport dynamics in the Solar System. Much research has been carried out in this area based on the paradigmatic case of the Circular Restricted Three-Body Problem. Many astrophysical systems, however, exhibit primaries in highly eccentric motion, thus requiring the adoption of the Elliptic Restricted Three-Body Problem (ERTBP) as a more appropriate reference model to accurately describe the dynamics of natural and possibly artificial bodies within them. The dynamical characteristics of the ERTBP, notably the absence of the Jacobi integral, the explicit time-dependence of the equations of motion in the synodical frame, the non-degeneracy of the spectrum of the periods of the periodic orbits, and the characteristics of the eigenvalues of the monodromy matrix, make it very different from its circular analogue. We have used Dynamical Systems Theory and associated numerical techniques to explore families of periodic orbits and their invariant manifolds aiming at the design of heteroclinic, low-energy transfer orbits in the framework of the Elliptic Restricted Three-Body Problem. An account will be given of the preliminary findings of this ongoing research. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Topputo FIRST NAME: Francesco BIRTH PLACE: Matera BIRTH DATE: 07/04/1978 AFFILIATION: Politecnico di Milano, Dipartimento di Ingegneria Aerospaziale e-MAIL: topputo@aero.polimi.it ARRIVAL DATE: 11/09/2005 DEPARTURE: 17/09/2005 SINGLE ROOM: NO DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: YES TITLE: Sixth-Order Linear Multi-Point Method: an Astrodynamical Application (F. Topputo, R. Armellin, L. P. Quartapelle) ABSTRACT: TPBVP (Two-Point Boundary Value Problem) arises when, solving a set of ODEs, conditions on the state variables are prescribed on both sides of the integration domain. Solving a TPBVP is a usual task in astrodynamics when a nominal trajectory is required with specified properties at its ends. A typical example occurs in preliminary mission analysis, in the frame of two-body problem, when looking for an arc linking two fixed points in a given time: this is the Lambert\'s problem. Such a problem can be solved by using efficient algorithms since an analytic solution is available in the case of a two-body model. In the present paper a sixth-order linear multipoint method (LMPM) has been derived to solve TPBVPs arising in more difficult models, as the three-body context, where the chaotic regime makes the TPBVP solution a more challenging task. The sixth-order accuracy is achieved by approximating the dynamical system over a uniform grid by means of general four-point computational molecules and two special five-point molecules defined at the two ends of the integration interval. The sixth-order LMPM attains accuracy beyond the first Dahlquist stability barrier since the integration scheme guarantees an order of accuracy of six while it is expected to be four from the Dahlquist’s theorem. The sixth-order Linear Multi-Point Method has been proven to be effective both for the computation of halo orbits and for the solution of Lambert like problem in the restricted three-body model. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: musso FIRST NAME: ivano BIRTH PLACE: cuneo italy BIRTH DATE: 11 feb 1975 AFFILIATION: isti-cnr pisa e-MAIL: ivano.musso@isti.cnr.it ARRIVAL DATE: tbd DEPARTURE: tbd SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Biscani FIRST NAME: Francesco BIRTH PLACE: Trento BIRTH DATE: 06/02/1980 AFFILIATION: University of Padova - Department of Astronomy e-MAIL: biscani@pd.astro.it ARRIVAL DATE: 10/09/2005 DEPARTURE: 17/09/2005 SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: YES TITLE: The Tidal Potential of Saturn and its Satellite System ABSTRACT: In this paper we present a new method for the development of the gravitational disturbing function acting on a mass located in a system of point-mass satellites moving along prescribed trajectories around a primary. The novelty of the method lies in its completely analytical approach to transforming the theories of the motion of the satellites into the coefficients of the tidal potential of the satellite system. The method is an extension of the one used by the authors to reproduce and extend Doodson\'s celebrated 1921 development for the Sun-Earth-Moon system using the rotation and translation theorems for spherical harmonic functions. This multi-body tidal potential development can be used for a quick assessment of the perturbation spectrum affecting the motion of a particle orbiting, or passing through the multi-satellite system or in computing the torques determining the rotational motion of bodies in the system (a prerequisite for the development of their precession and nutation series). It can also be used for geophysical or geodetic applications to system bodies, like the tidal displacement of their surfaces. In particular, the development has been carried out for the Saturnian satellite system because of the current interest in the Cassini mission, although applications of the present methodology to other satellite systems in the Solar System are also possible. A possible benefit of the present development is in the analysis of the motion of newly-discovered small moons and to the early planning phases of space missions. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Boccaletti FIRST NAME: Dino BIRTH PLACE: Correggio (RE) Italy BIRTH DATE: 8/6/1936 AFFILIATION: Università di Roma \"La Sapienza\" e-MAIL: boccaletti@uniroma1.it ARRIVAL DATE: 11/9/2005 DEPARTURE: 16/9/2005 SINGLE ROOM: yes DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Rambaux FIRST NAME: Nicolas BIRTH PLACE: Bordeaux (France) BIRTH DATE: 13-10-1976 AFFILIATION: University of Namur and Royal Observatory of Belgium (Belgium) e-MAIL: Nicolas.Rambaux@fundp.ac.be ARRIVAL DATE: 11-09-2005 DEPARTURE: 17-09-2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: TALK: YES TITLE: An accurate theory of the rotation of Mercury ABSTRACT: We have used the SONYR model of Bois and Rambaux (acronym of Spin-Orbit N-bodY Relativisitic model) of the solar System in order to reach a very accurate rotational motion of Mercury. The approach of the BJV model (Bois, Journet and Vockrouhlicky) as well as its SONYR extension derive from the DSX formulation of the post-Newtonian theory of motion for a system of N arbitrary extended, weakly self-graviting, rotating and deformable bodies in mutual interactions. As a consequence, the SONYR model gives an accurate simultaneous integration of the spin-orbit motion of Mercury. Moreover, the model includes the Mercury’s core-rotation couplings by the way of different internal structure models. The obtained rotation of Mercury is in agreement with the analytical theory of D’Hoedt and Lemaître. The SONYR theory of the Mercury’s rotation gives a complete analysis of the Mercury’s librations as well as the origin of the oscillation in its obliquity. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Chatzivantsidis FIRST NAME: Georgios BIRTH PLACE: Greece BIRTH DATE: 11/01/1975 AFFILIATION: PhD Student at Section of Astronomy, Astrophysics & Mechanics, Department of Physics - Aristotle University of Thessaloniki - Greece e-MAIL: hadjivan@astro.auth.gr ARRIVAL DATE: 10/11/2005 DEPARTURE: 17/11/2005 SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: YES TITLE: Stable chaos, local integrals of motion and lyapunov exponents in systems of 3 degrees of freedom. Application to the J12/7 resonance ABSTRACT: In previous works it was stated that stable chaos seemed to be associated with the existence of local integrals of motion in particular regions of the phase space. We support this hypothesis by calculating the full spectrum of the lyapunov exponents in such regions of the 3B-problem. Comparisons with the results of the estimation of the topological dimension of the trajectories in the 3-D embedding space of proper elements are also being made for the 12/7 resonance of an asteroid with Jupiter. POSTER: Yes POSTER TITLE: Stable chaos, local integrals of motion and lyapunov exponents in systems of 3 degrees of freedom. Application to the J12/7 resonance ABSTRACT: In previous works it was stated that stable chaos seemed to be associated with the existence of local integrals of motion in particular regions of the phase space. We support this hypothesis by calculating the full spectrum of the lyapunov exponents in such regions of the 3B-problem. Comparisons with the results of the estimation of the topological dimension of the trajectories in the 3-D embedding space of proper elements are also being made for the 12/7 resonance of an asteroid with Jupiter. ===================================================== LAST NAME: Muñoz-Almaraz FIRST NAME: Francisco Javier BIRTH PLACE: Sevilla (Spain) BIRTH DATE: 18/03/1973 AFFILIATION: Universitat de Barcelona e-MAIL: malmaraz@maia.ub.es ARRIVAL DATE: 10/09 DEPARTURE: 16/09 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Haw Wei Shiau TALK: YES TITLE: Families of symmetric periodic orbits in the three body problem and the figure eight. ABSTRACT: Chenciner and Montgomery have proved the existence of a solution (called figure eight) in the three body problem which is symmetric with several time-reversal symmetries. We state a theoretical result for the persistence of symmetric solutions with respect two time--reversal symmetries and we set a boundary value problem whose \"regular\" continuation is equivalent to the continuation of the symmetric solutions. This method is applied starting from the figure eight when one of the mass is varied. Several families of symmetric periodic orbits are got and the bifurcations undergo along this family allow us to explain different behauvior depending on the chosen symmetry. Subharmonic bifurcations are also considered. (Work joint with E. Freire, J. Galán and A. Vanderbauwhede) POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: MARTINOT FIRST NAME: VINCENT BIRTH PLACE: Saint-Dizier (France) BIRTH DATE: 19/07/1969 AFFILIATION: Alcatel Space e-MAIL: vincent.martinot@space.alcatel.fr ARRIVAL DATE: 11/09/2005 DEPARTURE: 16/09/2005 SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: YES TITLE: ABSTRACT: POSTER: NO POSTER TITLE: Visiting the Moons of Mars ABSTRACT: There have been several projects of visiting the Moons of Mars in the overall goal to better know Mars, some of them even envisaging to establish a first manned base on them. After presenting an overview of the contexts in which these projects were proposed, this article defines possible mission scenarios for a mission inspecting the Moon(s) of Mars, from the Earth departure to a close formation flying with the Moons. ===================================================== LAST NAME: Casotto FIRST NAME: Stefano BIRTH PLACE: Padova BIRTH DATE: 7-1-59 AFFILIATION: Università di Padova e-MAIL: casotto@pd.astro.it ARRIVAL DATE: 11-9 DEPARTURE: 16-9 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: no, ma coautore in De Pascale et al., Casotto Fantino Alessi, Casotto Biscani TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: robutel FIRST NAME: philippe BIRTH PLACE: tournan, France BIRTH DATE: 17 juin 1964 AFFILIATION: IMCCE, Observatoire de Paris. e-MAIL: robutel@imcce.fr ARRIVAL DATE: 11 DEPARTURE: 17 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: Diffusion in Jupiter’s Trojan swarm ABSTRACT: In a previous paper, we have shown the existence of a resonant web in the space phase of Jupiter’s Trojans. After a brief description of this resonant structure, we will show how it generates diffusion in the frequency space. Then, we will try to connect the diffusion to the long-term erosion of the Trojan’s swarm and its long-term stability. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Benettin FIRST NAME: Giancarlo BIRTH PLACE: Padova BIRTH DATE: 17/6/1948 AFFILIATION: Universita\' di Padova e-MAIL: benettin@math.unipd.it ARRIVAL DATE: 11/9/05 DEPARTURE: 15/9/05 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Makó FIRST NAME: Zoltán BIRTH PLACE: Sf. Gheorghe, Romania BIRTH DATE: 20 JUNE 1968 AFFILIATION: DEPARTMENT OF MATHEMATICS AND INFORMATICS, SAPIENTIA UNIVERSITY, 530104-Miercurea Ciuc, Romania e-MAIL: makozoltan@sapientia.siculorum.ro ARRIVAL DATE: 11 September 2005 DEPARTURE: 16 September 2005 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Szenkovits Ferenc TALK: YES TITLE: Hyperbolic structure of the capture domain ABSTRACT: Several authors studied the capture of small bodies by major planets, introducing different concepts of capture, like weak capture , temporary capture, longest capture, resonant capture, etc. In all these studies the time is used as measure of the capture. In this paper we try to study the phenomenon of capture using the variation of the angle Dj of the small body around the capturing planet. We defined the capture effect of the planet to the captured body, as the variation of the angle Dj during the capture, as long as the Kepler-energy of the small body relative to the central planet is negative. The beginning moment the capture is in the moment when the Kepler-energy of the captured body, relative to the capturing body, becomes negative. The end of capture is in the moment when the Kepler-energy becomes positive. The variation of capture effect around to Jupiter is studied using sections. We are determined several zones, in which, for a given velocity, the capture is occur. These regions we named capture domain. In this paper we show that the capture domain is chaotic, since this domain has a hyperbolic structure. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Galan-Vioue FIRST NAME: Jorge BIRTH PLACE: Sevilla Spain BIRTH DATE: 30-08-1966 AFFILIATION: Universidad de Sevilla e-MAIL: jgv@us.es ARRIVAL DATE: 10-9-2005 DEPARTURE: 16-9-2005 SINGLE ROOM: yes DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: yes TITLE: The principle of stationary action and the figure eight solution ABSTRACT: The existence of the figure eight solution of the three body problem was proven by minimizing the action integral over a restricted set of symmetric arcs. There has been a controversy about the stability of the real minimizer of the action. It is unclear whether the minimizer has to be elliptic or hyperbolic. From the variational point of view if the symmetry restriction is relaxed and we enlarge the space of arcs over which the action is minimized, then the value of the action cannot increase. In this talk we analyze the relation between the stability and the minimizing character of the solutions by studying the existence of conjugate points in this remarkable solution both in the planar and spatial case and other related problems. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Locatelli FIRST NAME: Ugo BIRTH PLACE: Bergamo BIRTH DATE: 26/05/1967 AFFILIATION: Dip. di Matematica, Universita\' di Roma \"Tor Vergata\" e-MAIL: locatell@mat.uniroma2.it ARRIVAL DATE: 11-12-13/9 DEPARTURE: 14-15-16/9 SINGLE ROOM: YES DOUBLE ROOM: YES POSSIBLY SHARED WITH: As you wish TALK: YES TITLE: Averaging over the \"fast frequency\" of the Trojan asteroids ABSTRACT: In a recent work by Gabern, Jorba and myself ([GJL], in press on Nonlinearity), we studied the stability of the Trojan asteroids in the framework of the planar circular restricted three-body problem. We succeeded in constructing the invariant tori well approximating the orbits in 23 over 30 considered cases, so that we largely improved the previously existing results. The construction of the invariant tori is based on a careful and quite technical reformulation of the Kolmogorov\'s normalization algorithm. It is well known that the motions very close to the Lagrangian points are characterized by two frequencies and one of them is much slower than the other one. In order to improve and simplify our approach, we first average the Hamiltonian over the faster frequency. This allow us to produce an integrable approximation of the system, which can be used as a new starting point for the construction of the invariant tori. The results of this new approach will be compared with those in [GJL]. POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Navarro Tapias-Fernando FIRST NAME: Montserrat BIRTH PLACE: Barcelona BIRTH DATE: 05/08/1977 AFFILIATION: Universitat de Barcelona e-MAIL: montse@maia.ub.es ARRIVAL DATE: 11/09 DEPARTURE: 18/09 SINGLE ROOM: No DOUBLE ROOM: Yes POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Merlo FIRST NAME: Olivier BIRTH PLACE: Liestal, Switzerland BIRTH DATE: 5/5/1969 AFFILIATION: Centro de Ciencias Fisicas, U.N.A.M., Cuernavaca, Mexico e-MAIL: merlo@quasar.unibas.ch ARRIVAL DATE: 11 DEPARTURE: 16 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: Yes TITLE: From Rotating billiards to narrow planetary rings ABSTRACT: POSTER: No POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Iess FIRST NAME: Luciano BIRTH PLACE: Padova BIRTH DATE: 8/5/58 AFFILIATION: Universita\' di Roma La Sapienza e-MAIL: iess@hermes.diaa.uniroma1.it ARRIVAL DATE: TBD DEPARTURE: TBD SINGLE ROOM: NO DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: YES TITLE: Invited Talk ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Waldvogel FIRST NAME: Joerg BIRTH PLACE: Zurich, Switzerland BIRTH DATE: 02/24/1938 AFFILIATION: Applied Mathematics, ETH FLI C3, CH-8092 Zurich e-MAIL: waldvogel@sam.math.ethz.ch ARRIVAL DATE: 09/11/2005 DEPARTURE: 09/17/2005 SINGLE ROOM: No DOUBLE ROOM: Yes POSSIBLY SHARED WITH: Irene Waldvogel, accompanying TALK: Yes TITLE: Quaternions and the perturbed Kepler problem ABSTRACT: Quaternions, introduced in 1856 by W. R. Hamilton as a generalization of complex numbers, lead to a remarkably simple representation of the perturbed three-dimensional Kepler problem in regularized variables. The talk gives an overview of this technique, including applications to perturbation theories. POSTER: No POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Barkin FIRST NAME: Yury BIRTH PLACE: Russia, Gorky Region BIRTH DATE: 23.04.51 AFFILIATION: Sternberg Astronomical Institute, Moscow e-MAIL: yuri.barkin@ua.es ARRIVAL DATE: 11.09.2005 DEPARTURE: 17.09.2005 SINGLE ROOM: Yes DOUBLE ROOM: No POSSIBLY SHARED WITH: TALK: No TITLE: ABSTRACT: POSTER: Yes POSTER TITLE: MERCURY: ROTATION, GRAVITATIONAL FIELD, ITS VARIATIONS ABSTRACT: MERCURY: ROTATION, GRAVITATIONAL FIELD, ITS VARIATIONS Barkin Yu.V.(1,2), Ferrandiz J.M(2) (1) Sternberg Astronomical Institute, Universitetskii pr-t, 13, Moscow, Russia, barkin@inbox.ru (2) Alicante University, Department of Applied Mathematics, San Vicente del Raspeig, Alicante, Spain The perturbation theory for Mercury rotation is developed for its rigid and two-layer models. The main regularities in the Mercury rotation – Cassini-Colombo laws were established and deduced from canonical equations of motion in Andoyer variables. The study has been fulfilled in assumption that Mercury moves on perturbed (real) orbit and in particular on evaluating elliptical orbit. The theoretical value of inclination of the angular momentum of Mercury relatively to normal to the orbit plane was determined as 1.607 arcmin, close to first Barkin’s determinations of this angle 1.24 and 1.67 arcmin in 1985. Periods of resonant librations were evaluated on analytical formulae and the liquid core contribution to these values has been studied. Solar tidal variations of parameters of second harmonic of Mercury gravitational field were evaluated in first. ===================================================== LAST NAME: LARA FIRST NAME: MARTIN BIRTH PLACE: SPAIN BIRTH DATE: 1960 AFFILIATION: REAL OBSERVATORIO DE LA ARMADA e-MAIL: mlara@roa.es ARRIVAL DATE: 11 DEPARTURE: 16 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: Asuncion Conde (ACCOMPANYING) TALK: NO TITLE: ABSTRACT: POSTER: YES POSTER TITLE: A high order analytical theory for spacecraft motion around Europa ABSTRACT: Hill’s equations can be used for approximating the dynamic behavior around many celestial bodies. When considering also the oblateness perturbation, the model closely reproduces the real dynamics of an orbiter around planetary satellites. Close to the planetary satellite the ratio rotation rate of the satellite to mean motion of the orbiter is small. When considering this ratio as a small parameter, the Coriolis effect is a first order perturbation, while the third body tidal attraction, and the oblateness perturbation remain at higher orders. We develope a fourth order theory that retains all the main features of the problem. Furthermore, with our theory we are able to relate the relative equilibria of the reduced problem with periodic solutions in a synodic frame ===================================================== LAST NAME: Namouni FIRST NAME: Fathi BIRTH PLACE: Annaba, Algeria BIRTH DATE: 23081969 AFFILIATION: CNRS, Observatoire de la cote d\'Azur e-MAIL: namouni@obs-nice.fr ARRIVAL DATE: 10092005 DEPARTURE: 15092005 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: On the Origin of the Eccentricities of Extrasolar Planets ABSTRACT: We present a phenomenological theory that aims to account for the origin of the large eccentricities of extrasolar planets and that of the small eccentricities in the solar system, the preference for apsidal alignment in non-resonant multiplanet systems, and the origin of the similarities in the eccentricity distribution of extrasolar planets and that of spectroscopic binary stars. We show that if a physical process is weakly dependent on the local dynamics of the companion and imparts a small relative acceleration to the star-companion system, the eccentricity of the companion\'s orbit is excited to large values depending on the direction and duration of acceleration. A natural candidate for such processes are asymmetric stellar jets and star-disk winds. The acceleration\'s strength is best constrained in multiplanet systems because of the companions\' mutual gravitational perturbations, while the acceleration\'s duration is bounded by the condition that the residual velocity imparted to the star is smaller than the stellar velocity dispersion in the Galaxy. In the outer parts of the star-companion system where the acceleration excitation time is comparable to or smaller than the orbital period, significant radial migration takes place which may have important consequences for the dynamics of the minor body populations in the solar system. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: LASKAR FIRST NAME: Jacques BIRTH PLACE: Paris BIRTH DATE: 28/04/1955 AFFILIATION: Observatoire de Paris, France e-MAIL: laskar@imcce.fr ARRIVAL DATE: 10 sept DEPARTURE: 17 sept SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: YES TITLE: Chaotic diffusion in the solar system ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Simula FIRST NAME: Alessandro BIRTH PLACE: Bergamo BIRTH DATE: 04-04-1966 AFFILIATION: EKAR - Altran e-MAIL: gio.vanna@iol.it ARRIVAL DATE: 12-09-2005 DEPARTURE: 16-09-2005 SINGLE ROOM: DOUBLE ROOM: yes POSSIBLY SHARED WITH: TALK: No TITLE: ABSTRACT: POSTER: No POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Villac FIRST NAME: Benjamin BIRTH PLACE: Perpignan BIRTH DATE: July 11, 1977 AFFILIATION: Jet Propulsion Laboratory e-MAIL: Benjamin.F.Villac@jpl.nasa.gov ARRIVAL DATE: Sept 11, 2005 DEPARTURE: Sept 17, 2005 SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: YES POSTER TITLE: Stability Maps, Unstable Periodic Orbits and Transfers in the Jupiter System ABSTRACT: Several examples of transfers between different Galilean moons in the Jupiter system, based on the transport mechanism offered by unstable periodic orbits and their associated stable/unstable manifolds and connections, are presented. The periodic orbits are obtained from stability maps based on a Fast Lyapunov Indicator. These maps also indicate the direction of the associated hyperbolic manifolds, giving spacecraft trajectory designers a quick method for locating low cost transfers using multi-body dynamics. ===================================================== LAST NAME: AMAR FIRST NAME: MAKHLOUF BIRTH PLACE: DREAN. ELTARF 36. ALGERIA BIRTH DATE: 31-08-56 AFFILIATION: dDepartment of mathematics-university of ANNABA-ALGERIA e-MAIL: makhloufamar@yahoo.fr ARRIVAL DATE: 10-09-05 DEPARTURE: 17-09-05 SINGLE ROOM: DOUBLE ROOM: yes POSSIBLY SHARED WITH: TALK: yes TITLE: Periodic solutions of Liénard systems ABSTRACT: Periodic solutions of Liénard systems MAKHLOUF AMAR Department of mathematics;University of Annaba.BP 12.Annaba.algeria. We consider the stability of critical points and the existence of limit cycles of two dimensionnal autonomous systems.We give conditions for systems to be globally asymptotically stable.We consider the polynomial Liénard systems and an application of Rychkov systems.We consider a perturbated Liénard system.We study the limit cycles in the weak and strongly nonlinear regime. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: AMAR FIRST NAME: MAKHLOUF BIRTH PLACE: DREAN. ELTARF 36. ALGERIA BIRTH DATE: 31-08-56 AFFILIATION: dDepartment of mathematics-university of ANNABA-ALGERIA e-MAIL: makhloufamar@yahoo.fr ARRIVAL DATE: 10-09-05 DEPARTURE: 17-09-05 SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: Periodic solutions of Liénard systems ABSTRACT: Periodic solutions of Liénard systems MAKHLOUF AMAR Department of mathematics;University of Annaba.BP 12.Annaba.algeria. We consider the stability of critical points and the existence of limit cycles of two dimensionnal autonomous systems.We give conditions for systems to be globally asymptotically stable.We consider the polynomial Liénard systems and an application of Rychkov systems.We consider a perturbated Liénard system.We study the limit cycles in the weak and strongly nonlinear regime. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: AMAR FIRST NAME: MAKHLOUF BIRTH PLACE: DREAN. ELTARF 36. ALGERIA BIRTH DATE: 31-08-56 AFFILIATION: dDepartment of mathematics-university of ANNABA-ALGERIA e-MAIL: makhloufamar@yahoo.fr ARRIVAL DATE: 10-09-05 DEPARTURE: 17-09-05 SINGLE ROOM: YES DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: yes TITLE: Periodic solutions of Liénard systems ABSTRACT: Periodic solutions of Liénard systems MAKHLOUF AMAR Department of mathematics;University of Annaba.BP 12.Annaba.algeria. We consider the stability of critical points and the existence of limit cycles of two dimensionnal autonomous systems.We give conditions for systems to be globally asymptotically stable.We consider the polynomial Liénard systems and an application of Rychkov systems.We consider a perturbated Liénard system.We study the limit cycles in the weak and strongly nonlinear regime. POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Lo FIRST NAME: Martin BIRTH PLACE: Taipei, Taiwan BIRTH DATE: Jan 7, 1953 AFFILIATION: Jet Propulsion Laboratory e-MAIL: Martin.Lo@jpl.nasa.gov ARRIVAL DATE: Sep 10 DEPARTURE: Sep 16 SINGLE ROOM: NO DOUBLE ROOM: YES POSSIBLY SHARED WITH: William Wentzel (Accomanying) TALK: NO TITLE: ABSTRACT: POSTER: YES POSTER TITLE: Trajectory Design for the SmallTug Mission ABSTRACT: The SmallTug mission is a technology demonstration for the NASA Space Exploration Program to show the usefulness of low energy trajectories for cargo transport between the Earth and the Moon. These trajectories are generated by the invariant manifolds of unstable quasiperiodic orbit in the Earth-Moon and Sun-Earth systems as coupled 3 body systems. By trading time for less fuel, such trajectories are ideal for the transport of cargo. The trajectory concept is based on previous work by the author on a Lunar Gateway Station concept. For the SmallTug, the trajectory starts with a Geostationary Transfer Orbit and uses low thrust transfer via invariant manifolds to place the microspacecraft in orbit about Lunar L1. After orbiting LL1 for several orbits, the spacecraft will be brought back to Earth orbit to demonstrate the feasibility of this concept. Invariant manifolds continue to play a key role even in the low thrust trajectory domain. ===================================================== LAST NAME: DUFEY FIRST NAME: JULIEN BIRTH PLACE: belgium BIRTH DATE: 27/06/83 AFFILIATION: University of Namur - Belgium e-MAIL: dufey@math.ucl.ac.be ARRIVAL DATE: 11/09/05 DEPARTURE: 17/09/05 SINGLE ROOM: DOUBLE ROOM: yes POSSIBLY SHARED WITH: see email TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Sathe FIRST NAME: Dileep BIRTH PLACE: Pune BIRTH DATE: 16 August 1947 AFFILIATION: Dadawala Jr. College - retiring on 31 August 2005 e-MAIL: dileepsathe@vsnl.net ARRIVAL DATE: 9th Sept. DEPARTURE: 17th Sept. SINGLE ROOM: Yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: Yes TITLE: Planetary motion: Why is it still difficult to learn? ABSTRACT: Sending separately. POSTER: NO POSTER TITLE: xxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxx ABSTRACT: xxxxxxxxxxxxxxxxxxxxxxx ===================================================== LAST NAME: Ajadi FIRST NAME: Shola Ezekiel BIRTH PLACE: Port-Harcourt BIRTH DATE: 02 /04 /1975 AFFILIATION: Organisation e-MAIL: ajadius@yahoo.com ARRIVAL DATE: 10 sept 2005 DEPARTURE: 17 sept 2005 SINGLE ROOM: No DOUBLE ROOM: Yes POSSIBLY SHARED WITH: sayo jokotoye accompanying person TALK: No TITLE: N/A ABSTRACT: n/A POSTER: No POSTER TITLE: n/a ABSTRACT: n/a ===================================================== LAST NAME: PALEARI FIRST NAME: SIMONE BIRTH PLACE: MILANO BIRTH DATE: 9.11.72 AFFILIATION: Dipartimento di Matematica e Applicazioni -- Universita\' di Milano Bicocca e-MAIL: simone.paleari@unimib.it ARRIVAL DATE: 11.9.05 DEPARTURE: 16.9.05 SINGLE ROOM: yes DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Costa FIRST NAME: Claudio BIRTH PLACE: Roma BIRTH DATE: 9 Nov 1955 AFFILIATION: Unione Astrofili Italiani e-MAIL: c.costa@mclink.it ARRIVAL DATE: 11 Set 2005 DEPARTURE: 16 Set 2005 SINGLE ROOM: No DOUBLE ROOM: No POSSIBLY SHARED WITH: TALK: No TITLE: ABSTRACT: POSTER: No POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: OKAFOR FIRST NAME: IWUCHUKWU DAVID BIRTH PLACE: NIGERIA BIRTH DATE: 26/10/1985 AFFILIATION: LSMC e-MAIL: davaldo007@yahoo.com ARRIVAL DATE: SEP DEPARTURE: SEP SINGLE ROOM: YES DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: AMOROSI FIRST NAME: LUCIA BIRTH PLACE: ROMA BIRTH DATE: 28/07/71 AFFILIATION: ALCATEL ALENIA SPACE ITALIA e-MAIL: lucia.amorosi@aleniaspazio.it ARRIVAL DATE: 12/09/05 DEPARTURE: 16/09/05 SINGLE ROOM: NO DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Sollazzo FIRST NAME: Loredana BIRTH PLACE: Gragnano (NA) BIRTH DATE: 22.01.1974 AFFILIATION: Alcatel Alenia Space Italia e-MAIL: loredana.sollazzo@aleniaspazio.it ARRIVAL DATE: 12.09.2005 DEPARTURE: 16.09.2005 SINGLE ROOM: NO DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Notarantonio FIRST NAME: Anna BIRTH PLACE: Pescasseroli BIRTH DATE: 04-Jan-1954 AFFILIATION: Alcatel Alenia Space Italia e-MAIL: anna.notarantonio@aleniaspazio.it ARRIVAL DATE: 12-Sep-2005 DEPARTURE: 12-Sep-2005 SINGLE ROOM: NO DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Notarantonio FIRST NAME: Anna BIRTH PLACE: Pescasseroli BIRTH DATE: 04-Jan-1954 AFFILIATION: Alcatel Alenia Space Italia e-MAIL: anna.notarantonio@aleniaspazio.it ARRIVAL DATE: 12-Sep-2005 DEPARTURE: 16-Sep-2005 SINGLE ROOM: NO DOUBLE ROOM: NO POSSIBLY SHARED WITH: TALK: NO TITLE: ABSTRACT: POSTER: NO POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: Owis FIRST NAME: Ashraf BIRTH PLACE: Giza-Egypt BIRTH DATE: 26/2/1975 AFFILIATION: Milano-Bicocca University e-MAIL: ashraf.owis@unimib.it ARRIVAL DATE: 11/9/2005 DEPARTURE: 16/9/2005 SINGLE ROOM: yes DOUBLE ROOM: no POSSIBLY SHARED WITH: TALK: no TITLE: ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: ad FIRST NAME: ad BIRTH PLACE: da BIRTH DATE: da AFFILIATION: da e-MAIL: namouni@yahoo.com ARRIVAL DATE: ads DEPARTURE: dad SINGLE ROOM: a DOUBLE ROOM: a POSSIBLY SHARED WITH: a TALK: a TITLE: a ABSTRACT: qeq POSTER: aa POSTER TITLE: aa ABSTRACT: qed ===================================================== LAST NAME: gronchi FIRST NAME: giovanni BIRTH PLACE: pisa BIRTH DATE: 21/03/1970 AFFILIATION: univ. pisa e-MAIL: gronchi@dm.unipi.it ARRIVAL DATE: 1/1/1999 DEPARTURE: 1/1/2000 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: tit ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: gronchi FIRST NAME: giovanni BIRTH PLACE: pisa BIRTH DATE: 21/03/1970 AFFILIATION: univ. pisa e-MAIL: gronchi@dm.unipi.it ARRIVAL DATE: 1/1/1999 DEPARTURE: 1/1/2000 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: tit ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: ===================================================== LAST NAME: gronchi FIRST NAME: giovanni federico BIRTH PLACE: pisa BIRTH DATE: 21/03/1970 AFFILIATION: univ. Pisa e-MAIL: gronchi@dm.unipi.it ARRIVAL DATE: 1/1/1999 DEPARTURE: 1/2/2000 SINGLE ROOM: yes DOUBLE ROOM: POSSIBLY SHARED WITH: TALK: yes TITLE: title ABSTRACT: POSTER: no POSTER TITLE: ABSTRACT: =====================================================