The space missions MESSENGER and BepiColombo require precise short-term studies of Mercury's ... more The space missions MESSENGER and BepiColombo require precise short-term studies of Mercury's rotation. In this scope, we perform analytically and numerically by Hamiltonian approach a synthetic 2-dimensional representation of its rotation, using complete ephemerides of the orbital motions of the planets of the Solar System. This representation allows us to derive the librations in longitude and latitude of the resonant
With the space missions MESSENGER and BepiColombo, there has been a renewed interest for Mercury.... more With the space missions MESSENGER and BepiColombo, there has been a renewed interest for Mercury. In this framework, we study the longitudinal and latitudinal librations of a 2-layer Mercury. We apply Hamiltonian mechanics to determine the effects of planetary perturbations on the librations (using both analytical and numerical methods). The libration in longitude is dominated by the 88-day and 11.86-year
The Saturnian coorbital satellites Janus and Epimetheus present a unique dynamical configuration ... more The Saturnian coorbital satellites Janus and Epimetheus present a unique dynamical configuration in the Solar System, because of high-amplitude horseshoe orbits, due to a mass ratio of order unity. As a consequence, they swap their orbits every 4 years, while their orbital periods is about 0.695 days. Recently, Tiscareno et al.(2009) got observational informations on the shapes and the rotational
Like our Moon, the majority of the solar system's... more Like our Moon, the majority of the solar system's satellites are locked in a 1:1 spin-orbit resonance; on average, these satellites show the same face toward the planet at a constant rotation rate equal to the satellite's orbital rate. In addition to the uniform rotational motion, physical librations (oscillations about an equilibrium) also occur. The librations may contain signatures of the satellite's internal properties. Using stereophotogrammetry on Cassini Image Science Subsystem (ISS) images, we measured longitudinal physical forced librations of Saturn's moon Mimas. Our measurements confirm all the libration amplitudes calculated from the orbital dynamics, with one exception. This amplitude depends mainly on Mimas' internal structure and has an observed value of twice the predicted one, assuming hydrostatic equilibrium. After considering various possible interior models of Mimas, we argue that the satellite has either a large nonhydrostatic interior, or a hydrostatic one with an internal ocean beneath a thick icy shell.
Campaign of observations of mutual events are organized regularly by the IMCCE: since 1979 for th... more Campaign of observations of mutual events are organized regularly by the IMCCE: since 1979 for the PHEMU campaign of the Galilean satellites and since 1995 for the PHESAT campaign of the Saturnian satellites. These observations are useful in order to detect tidal effects in the planet and in the satellites because they lead to very accurate positions. We describe mutual
We have observed the four Galilean satellites of Jupiter during their mutual occultations and ecl... more We have observed the four Galilean satellites of Jupiter during their mutual occultations and eclipses from February to April 2003 using a CCD camera attached to the 32.5cm refractor of the observatory of Lille. We have recorded 13 lightcurves of these events. We have performed a first astrometric reduction based on the method developed in Noyelles et al. (2003A&A...401.1159N). This
We present a 3-degree of freedom theory of Titan's forced rotation, as a rigid body. Such a s... more We present a 3-degree of freedom theory of Titan's forced rotation, as a rigid body. Such a study is possible thanks to the Cassini data of the gravitational potential of Titan. We use a semi-analytical model based on the recent analytical works of Henrard & Schwanen (2004), on a numerical integration and on an identification of the arguments as an
There is in the Jovian system a great inequality 3:7 between the satellites Ganymede and Callisto... more There is in the Jovian system a great inequality 3:7 between the satellites Ganymede and Callisto. This study aims at exploring the effects of this great inequality on the recent orbital history of the Galilean satellites. We found that the system has crossed several stochastic layers and have some candidates to former resonances who might have been disrupted by the
The dynamical history of Galilean satellites has been studied several times in order to explain t... more The dynamical history of Galilean satellites has been studied several times in order to explain the capture into the laplacian resonance. None of them includes the influence of De Haerdtl's inequality 3:7 between Ganymede and Callisto. This study aims at exploring the role played by this great inequality in the recent past, when tidal effects made the system cross the
The quasi-commensurability 7:3 between the mean motions of the Galilean satellites Ganymede and C... more The quasi-commensurability 7:3 between the mean motions of the Galilean satellites Ganymede and Callisto, known as De Haerdtl inequality, has never been taken into account in the scenarii of dynamical evolution of the Galilean satellites. We used numerical tools like frequency maps to detect the chaos induced by the inequality. We showed that it induces chaos, more particularly because of
We examine the problem of detecting the observational signature of tides in the Saturnian system.... more We examine the problem of detecting the observational signature of tides in the Saturnian system. We show that, because of energy transfer encouraged by the mean-motion resonances, S-1 Mimas' secular acceleration should be detected by observing S-3 Tethys instead of Mimas itself. We have a similar conclusion for the Enceladus/Dione resonance. We also show that detecting secular accelerations of these
Tidal dissipation inside gaseous planets is crucial for the study of their long term evolution. F... more Tidal dissipation inside gaseous planets is crucial for the study of their long term evolution. For the exo-planets tidal dissipation has often been estimated from the Solar system giant planets. The tidal dissipation inside Saturn and Jupiter can be determined from theoretical assumptions on the orbital evolution of their satellites. This provides a lower bound for their dissipation parameter Q.
The space missions MESSENGER and BepiColombo require precise short-term studies of Mercury's ... more The space missions MESSENGER and BepiColombo require precise short-term studies of Mercury's rotation. In this scope, we perform analytically and numerically by Hamiltonian approach a synthetic 2-dimensional representation of its rotation, using complete ephemerides of the orbital motions of the planets of the Solar System. This representation allows us to derive the librations in longitude and latitude of the resonant
With the space missions MESSENGER and BepiColombo, there has been a renewed interest for Mercury.... more With the space missions MESSENGER and BepiColombo, there has been a renewed interest for Mercury. In this framework, we study the longitudinal and latitudinal librations of a 2-layer Mercury. We apply Hamiltonian mechanics to determine the effects of planetary perturbations on the librations (using both analytical and numerical methods). The libration in longitude is dominated by the 88-day and 11.86-year
The Saturnian coorbital satellites Janus and Epimetheus present a unique dynamical configuration ... more The Saturnian coorbital satellites Janus and Epimetheus present a unique dynamical configuration in the Solar System, because of high-amplitude horseshoe orbits, due to a mass ratio of order unity. As a consequence, they swap their orbits every 4 years, while their orbital periods is about 0.695 days. Recently, Tiscareno et al.(2009) got observational informations on the shapes and the rotational
Like our Moon, the majority of the solar system's... more Like our Moon, the majority of the solar system's satellites are locked in a 1:1 spin-orbit resonance; on average, these satellites show the same face toward the planet at a constant rotation rate equal to the satellite's orbital rate. In addition to the uniform rotational motion, physical librations (oscillations about an equilibrium) also occur. The librations may contain signatures of the satellite's internal properties. Using stereophotogrammetry on Cassini Image Science Subsystem (ISS) images, we measured longitudinal physical forced librations of Saturn's moon Mimas. Our measurements confirm all the libration amplitudes calculated from the orbital dynamics, with one exception. This amplitude depends mainly on Mimas' internal structure and has an observed value of twice the predicted one, assuming hydrostatic equilibrium. After considering various possible interior models of Mimas, we argue that the satellite has either a large nonhydrostatic interior, or a hydrostatic one with an internal ocean beneath a thick icy shell.
Campaign of observations of mutual events are organized regularly by the IMCCE: since 1979 for th... more Campaign of observations of mutual events are organized regularly by the IMCCE: since 1979 for the PHEMU campaign of the Galilean satellites and since 1995 for the PHESAT campaign of the Saturnian satellites. These observations are useful in order to detect tidal effects in the planet and in the satellites because they lead to very accurate positions. We describe mutual
We have observed the four Galilean satellites of Jupiter during their mutual occultations and ecl... more We have observed the four Galilean satellites of Jupiter during their mutual occultations and eclipses from February to April 2003 using a CCD camera attached to the 32.5cm refractor of the observatory of Lille. We have recorded 13 lightcurves of these events. We have performed a first astrometric reduction based on the method developed in Noyelles et al. (2003A&A...401.1159N). This
We present a 3-degree of freedom theory of Titan's forced rotation, as a rigid body. Such a s... more We present a 3-degree of freedom theory of Titan's forced rotation, as a rigid body. Such a study is possible thanks to the Cassini data of the gravitational potential of Titan. We use a semi-analytical model based on the recent analytical works of Henrard & Schwanen (2004), on a numerical integration and on an identification of the arguments as an
There is in the Jovian system a great inequality 3:7 between the satellites Ganymede and Callisto... more There is in the Jovian system a great inequality 3:7 between the satellites Ganymede and Callisto. This study aims at exploring the effects of this great inequality on the recent orbital history of the Galilean satellites. We found that the system has crossed several stochastic layers and have some candidates to former resonances who might have been disrupted by the
The dynamical history of Galilean satellites has been studied several times in order to explain t... more The dynamical history of Galilean satellites has been studied several times in order to explain the capture into the laplacian resonance. None of them includes the influence of De Haerdtl's inequality 3:7 between Ganymede and Callisto. This study aims at exploring the role played by this great inequality in the recent past, when tidal effects made the system cross the
The quasi-commensurability 7:3 between the mean motions of the Galilean satellites Ganymede and C... more The quasi-commensurability 7:3 between the mean motions of the Galilean satellites Ganymede and Callisto, known as De Haerdtl inequality, has never been taken into account in the scenarii of dynamical evolution of the Galilean satellites. We used numerical tools like frequency maps to detect the chaos induced by the inequality. We showed that it induces chaos, more particularly because of
We examine the problem of detecting the observational signature of tides in the Saturnian system.... more We examine the problem of detecting the observational signature of tides in the Saturnian system. We show that, because of energy transfer encouraged by the mean-motion resonances, S-1 Mimas' secular acceleration should be detected by observing S-3 Tethys instead of Mimas itself. We have a similar conclusion for the Enceladus/Dione resonance. We also show that detecting secular accelerations of these
Tidal dissipation inside gaseous planets is crucial for the study of their long term evolution. F... more Tidal dissipation inside gaseous planets is crucial for the study of their long term evolution. For the exo-planets tidal dissipation has often been estimated from the Solar system giant planets. The tidal dissipation inside Saturn and Jupiter can be determined from theoretical assumptions on the orbital evolution of their satellites. This provides a lower bound for their dissipation parameter Q.
Uploads
Papers by B. Noyelles