Search

Your search keyword '"Noyelles, B"' showing total 39 results
Start Over Author "Noyelles, B"
39 results on '"Noyelles, B"'

1. Volatile-rich comets ejected early on during Solar System formation

Author

Anderson, S. E., Petit, J. -M., Noyelles, B., Mousis, O., and Rousselot, P.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Comet C/2016 R2 PanSTARRS (hereafter C/2016 R2) presents an unusually high N2/CO abundance ratio, as well as a heavy depletion in H2O, making it the only known comet of its kind. Understanding its dynamical history is therefore of essential importance as it would allow us to gain a clearer understanding of the evolution of planetesimal formation in our Solar System. Two studies have independently estimated the possible origin of this comet from building blocks formed in a peculiar region of the protoplanetary disk, near the ice line of CO and N2. We intend to investigate the fates of objects formed from the building blocks in these regions. We hope to find a possible explanation for the lack of C/2016 R2-like comets in our Solar System. Using a numerical simulation of the early stages of Solar System formation, we track the dynamics of these objects in the Jumping Neptune scenario based on five different initial conditions for the protosolar disk. We integrate the positions of 250 000 planetesimals over time in order to analyze the evolution of their orbits and create a statistical profile of their expected permanent orbit. Results. We find that objects formed in the region of the CO- and N2- ice lines are highly likely to be sent towards the Oort Cloud or possibly ejected from the Solar System altogether on a relatively short timescale. In all our simulations, over 90% of clones formed in this region evolved into a hyperbolic trajectory, and between 1% and 10% were potentially captured by the Oort Cloud. The handful of comets that remained were either on long-period, highly eccentric orbits like C/2016 R2, or absorbed into the Edgeworth-Kuiper belt. Comets formed <15 au were predominantly ejected early in the formation timeline. As this is the formation zone likely to produce comets of this composition, this process could explain the lack of similar comets observed in the Solar System, Comment: 7 pages, 5 figures

Published
2022
Full Text
View/download PDF

4. Equilibrium search algorithm of a perturbed quasi-integrable system

Author

Noyelles, B., Delsate, N., and Carletti, T.

Subjects
Mathematics - Dynamical Systems
Abstract

We hereby introduce and study an algorithm able to search for initial conditions corresponding to orbits presenting forced oscillations terms only, namely to completely remove the free or proper oscillating part. This algorithm is based on the Numerical Analysis of the Fundamental Frequencies algorithm by J. Laskar, for the identification of the free and forced oscillations, the former being iteratively removed from the solution by carefully choosing the initial conditions. We proved the convergence of the algorithm under suitable assumptions, satisfied in the Hamiltonian framework whenever the d'Alembert characteristic holds true. In this case, with polar canonical variables, we also proved that this algorithm converges quadratically. We provided a relevant application: the forced prey-predator problem., Comment: submitted to Physica D

Published
2011

5. Core-mantle interactions for Mercury

Author

Noyelles, B., Dufey, J., and Lemaitre, A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Mercury is the target of two space missions: MESSENGER (NASA) which orbit insertion is planned for March 2011, and ESA/JAXA BepiColombo, that should be launched in 2014. Their instruments will observe the surface of the planet with a high accuracy (about 1 arcsec for BepiColombo), what motivates studying its rotation. Mercury is assumed to be composed of a rigid mantle and an at least partially molten core. We here study the influence of the core-mantle interactions on the rotation perturbed by the solar gravitational interaction, by modeling the core as an ellipsoidal cavity filled with inviscid fluid of constant uniform density and vorticity. We use both analytical (Lie transforms) and numerical tools to study this rotation, with different shapes of the core. We express in particular the proper frequencies of the system, because they characterize the response of Mercury to the different solicitations, due to the orbital motion of Mercury around the Sun. We show that, contrary to its size, the shape of the core cannot be determined from observations of either longitudinal or polar motions. However, we highlight the strong influence of a resonance between the proper frequency of the core and the spin of Mercury that raises the velocity field inside the core. We show that the key parameter is the polar flattening of the core. This effect cannot be directly derived from observations of the surface of Mercury, but we cannot exclude the possibility of an indirect detection by measuring the magnetic field., Comment: MNRAS, in press

Published
2010
Full Text
View/download PDF

6. Theory of the rotation of Janus and Epimetheus

Author

Noyelles, B.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

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 states of these satellites. In particular, they detected an offset in the expected equilibrium position of Janus, and a large libration of Epimetheus. We here propose to give a 3-dimensional theory of the rotation of these satellites in using these observed data, and to compare it to the observed rotations. We consider the two satellites as triaxial rigid bodies, and we perform numerical integrations of the system in assuming the free librations as damped. The periods of the three free librations we get, associated with the 3 dimensions, are respectively 1.267, 2.179 and 2.098 days for Janus, and 0.747, 1.804 and 5.542 days for Epimetheus. The proximity of 0.747 days to the orbital period causes a high sensitivity of the librations of Epimetheus to the moments of inertia. Our theory explains the amplitude of the librations of Janus and the error bars of the librations of Epimetheus, but not an observed offset in the orientation of Janus., Comment: Accepted for publication in Icarus

Published
2009
Full Text
View/download PDF

7. Titan's rotation: A 3-dimensional theory

Author

Noyelles, B., Lemaitre, A., and Vienne, A.

Subjects
Astrophysics
Abstract

We study the forced rotation of Titan seen as a rigid body at the equilibrium Cassini state, involving the spin-orbit synchronization. We used both the analytical and the numerical ways. We analytically determined the equilibrium positions and the frequencies of the 3 free librations around it, while a numerical integration associated to frequency analysis gave us a more synthetic, complete theory, where the free solution split from the forced one. We find a mean obliquity of 2.2 arcmin and the fundamental frequencies of the free librations of about 2.0977, 167.4883, and 306.3360 years. Moreover, we bring out the main role played by Titan's inclination on its rotation, and we suspect a likely resonance involving Titan's wobble., Comment: accepted for publication in Astronomy ans Astrophysics

Published
2007
Full Text
View/download PDF

8. Titan's rotational state : The effects of a forced 'free' resonant wobble

Author

Noyelles, B.

Subjects
Astrophysics
Abstract

In Noyelles et al. (2008, Astron. Astrophys., 478, 959-970), a resonance involving the wobble of Titan is hinted. This paper studies this scenario and its consequences. The first step is to build an accurate analytical model that would help to find the likely resonances in the rotation of every synchronous body. In this model, I take the orbital eccentricity of the body into account, as well as its variable inclination with respect to Saturn's equator. Then an analytical study using the second fundamental model of the resonance is performed to study the resonance of interest. Finally, I study the dissipative consequences of this resonance. I find that this resonance may have increased the wobble of Titan by several degrees. For instance, if Titan's polar momentum C is equal to 0.355MR_T^2 (M and R_T being respectively Titan's mass and radius), the wobble might be forced to 41 degrees. Thanks to an original formula, I find that the dissipation associated with the forced wobble might not be negligible compared to the contribution of the eccentricity. I also suspect that, due to the forced wobble, Titan's period of rotation may be somewhat underestimated by observers. Finally, I use the analytical model presented in this paper to compute the periods of the free librations of the four Galilean satellites as well as the Saturnian satellite Rhea. For Io and Europa, the results are consistent with previous studies. For the other satellites, the periods of the free librations are respectively 186.37 d, 23.38 y and 30.08 y for Ganymede, 2.44 y, 209.32 y and 356.54 y for Callisto, and 51.84 d, 2.60 y and 3.59 y for Rhea., Comment: accepted for publication in Celestial Mechanics and Dynamical Astronomy

Published
2007
Full Text
View/download PDF

9. N2/CO ratio in comets insensitive to orbital evolution.

Author

Anderson, S E, Rousselot, P, Noyelles, B, Jehin, E, and Mousis, O

Subjects
COMETS, SOLAR system, HALLEY'S comet, PROTOPLANETARY disks
Abstract

Comets are seen as depleted in nitrogen compared to the protosolar value, but a small number exhibit significantly higher than typical N2/CO ratios: C/1908 R1 (Morehouse), C/1940 R2 (Cunningham), C/1947 S1 (Bester), C/1956 R1 (Arend–Roland), C/1957 P1 (Mrkos), C/1961 R1 (Humason), C/1969 Y1 (Bennett), C/1973 E1 (Kohoutek), C/1975 V1-A (West), C/1986 P1 (Wilson), C/1987 P1 (Bradfield), C/2001 Q4 (NEAT), C/2002 VQ94 (LINEAR), C/2016 R2 (PanSTARRS), and periodic comets 1P/Halley, 29P/Schwassmann–Wachmann 1, and 67P/Churyumov–Gerasimenko. This study examines the composition and dynamical histories of these N2-'rich' comets to unearth insights into their formation processes. Using updated N2 fluorescence factors, we re-estimate the N2/CO ratios of this sample and find that they are consistent with the expected values for comets based on estimations of the protosolar nebula. These also often display larger nucleus sizes and show rapid tail morphology variations due to their ionic nature. Numerical simulations reveal no common dynamical history, suggesting that the N2/CO ratio is independent of the number of inner Solar System passages and that N2 is homogeneously distributed within these comets. These volatile-rich comets share an Oort Cloud origin which is consistent with their survival over the past 4.5 Gyr. Our study also suggests that there may be a bias using modern high-resolution spectrometers with narrow slits, which could potentially overlook the ion tail of comets. We advocate for the use of long-slit spectroscopy to potentially detect a wider range of N2-rich comets, thereby enriching our understanding of comet compositions and origins. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

10. The science case for an orbital mission to Uranus: Exploring the origins and evolution of ice giant planets

Author

Arridge, C.S., Achilleos, N., Agarwal, J., Agnor, C.B., Ambrosi, R., André, N., Badman, S.V., Baines, K., Banfield, D., Barthélémy, M., Bisi, M.M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalié, T., Christophe, B., Coates, A.J., Collinson, G., Cooper, J.F., Costa-Sitja, M., Courtin, R., Daglis, I.A., de Pater, I., Desai, M., Dirkx, D., Dougherty, M.K., Ebert, R.W., Filacchione, G., Fletcher, L.N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grün, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J.K., Hofstadter, M.H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C.M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Krüger, H., Kurth, W.S., Labrianidis, C., Lainey, V., Lamy, L.L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J.I., Mousis, O., Nettelmann, N., Neubauer, F.M., Nordheim, T., Noyelles, B., Orton, G.S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C.T., Rymer, A.M., Sallantin, R., Sánchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, K.M., Schenk, P., Schubert, J., Sergis, N., Sittler, E.C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E.P., Vinatier, S., Wilson, R., and Zarka, P.

Published
2014
Full Text
View/download PDF

16. N2 production rate in comet C/2016 R2 (PanSTARRS).

Author

Anderson, S E, Rousselot, P, Noyelles, B, Opitom, C, Jehin, E, Hutsemékers, D, and Manfroid, J

Subjects
NITROGEN, COMETS, FLUORESCENCE, DAUGHTERS
Abstract

Observations of comet C/2016 R2 (PanSTARRS) have revealed exceptionally bright emission bands of N |$_2^+$|⁠ , the strongest ever observed in a comet spectrum. Alternatively, it appears to be poor in CN compared to other comets, and remarkably depleted in H2O. Here, we quantify the N2 production rate from N |$_2^+$| emission lines using the Haser model. We derived effective parent and daughter scale lengths for N2 producing N |$_2^+$|⁠. This is the first direct measurement of such parameters. Using a revised fluorescence efficiency for N |$_2^+$|⁠ , the resulting production rate of molecular nitrogen is inferred to be Q(N2) ∼ 1 × 1028 molecules s−1 on average for 2018 February 11, 12, and 13, the highest for any known comet. Based on a CO production rate of Q(CO) ∼ 1.1 × 1029 molecules s−1, we find Q(N2)/Q(CO) ∼ 0.09, which is consistent with the N |$_2^+$| /CO+ ratio derived from the observed intensities of N |$_2^+$| and CO+ emission lines. We also measure significant variations in this production rate between our three observing nights, with Q(N2) varying by plus or minus 20 per cent according to the average value. [ABSTRACT FROM AUTHOR]

Published
2022
Full Text
View/download PDF

21. The science case for an orbital mission to Uranus: Exploring the origins and evolution of ice giant planets

Author

Arridge, C.S. Achilleos, N. Agarwal, J. Agnor, C.B. Ambrosi, R. André, N. Badman, S.V. Baines, K. Banfield, D. Barthélémy, M. Bisi, M.M. Blum, J. Bocanegra-Bahamon, T. Bonfond, B. Bracken, C. Brandt, P. Briand, C. Briois, C. Brooks, S. Castillo-Rogez, J. Cavalié, T. Christophe, B. Coates, A.J. Collinson, G. Cooper, J.F. Costa-Sitja, M. Courtin, R. Daglis, I.A. De Pater, I. Desai, M. Dirkx, D. Dougherty, M.K. Ebert, R.W. Filacchione, G. Fletcher, L.N. Fortney, J. Gerth, I. Grassi, D. Grodent, D. Grün, E. Gustin, J. Hedman, M. Helled, R. Henri, P. Hess, S. Hillier, J.K. Hofstadter, M.H. Holme, R. Horanyi, M. Hospodarsky, G. Hsu, S. Irwin, P. Jackman, C.M. Karatekin, O. Kempf, S. Khalisi, E. Konstantinidis, K. Krüger, H. Kurth, W.S. Labrianidis, C. Lainey, V. Lamy, L.L. Laneuville, M. Lucchesi, D. Luntzer, A. MacArthur, J. Maier, A. Masters, A. McKenna-Lawlor, S. Melin, H. Milillo, A. Moragas-Klostermeyer, G. Morschhauser, A. Moses, J.I. Mousis, O. Nettelmann, N. Neubauer, F.M. Nordheim, T. Noyelles, B. Orton, G.S. Owens, M. Peron, R. Plainaki, C. Postberg, F. Rambaux, N. Retherford, K. Reynaud, S. Roussos, E. Russell, C.T. Rymer, A.M. Sallantin, R. Sánchez-Lavega, A. Santolik, O. Saur, J. Sayanagi, K.M. Schenk, P. Schubert, J. Sergis, N. Sittler, E.C. Smith, A. Spahn, F. Srama, R. Stallard, T. Sterken, V. Sternovsky, Z. Tiscareno, M. Tobie, G. Tosi, F. Trieloff, M. Turrini, D. Turtle, E.P. Vinatier, S. Wilson, R. Zarka, P.

Subjects
Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics
Abstract

Giant planets helped to shape the conditions we see in the Solar System today and they account for more than 99% of the mass of the Sun's planetary system. They can be subdivided into the Ice Giants (Uranus and Neptune) and the Gas Giants (Jupiter and Saturn), which differ from each other in a number of fundamental ways. Uranus, in particular is the most challenging to our understanding of planetary formation and evolution, with its large obliquity, low self-luminosity, highly asymmetrical internal field, and puzzling internal structure. Uranus also has a rich planetary system consisting of a system of inner natural satellites and complex ring system, five major natural icy satellites, a system of irregular moons with varied dynamical histories, and a highly asymmetrical magnetosphere. Voyager 2 is the only spacecraft to have explored Uranus, with a flyby in 1986, and no mission is currently planned to this enigmatic system. However, a mission to the uranian system would open a new window on the origin and evolution of the Solar System and would provide crucial information on a wide variety of physicochemical processes in our Solar System. These have clear implications for understanding exoplanetary systems. In this paper we describe the science case for an orbital mission to Uranus with an atmospheric entry probe to sample the composition and atmospheric physics in Uranus' atmosphere. The characteristics of such an orbiter and a strawman scientific payload are described and we discuss the technical challenges for such a mission. This paper is based on a white paper submitted to the European Space Agency's call for science themes for its large-class mission programme in 2013. © 2014 Elsevier Ltd.

Published
2014

22. The science case for an orbital mission to Uranus: Exploring the origins and evolution of ice giant planets

Author

Arridge, C. S., Achilleos, N., Agarwal, J., Agnor, C. B., Ambrosi, R., Andre, N., Badman, S. V., Baines, K., Banfield, D., Barthelemy, M., Bisi, M. M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B. ., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalie, T., Christophe, B., Coates, A. J., Collinson, G., Cooper, J. F., Costa-Sitja, M., Courtin, R., Daglis, I. A., De Pater, I., Desai, M., Dirkx, D., Dougherty, M. K., Ebert, R. W., Filacchione, G., Fletcher, L. N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grun, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J. K., Hofstadter, M. H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C. M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Kruger, H., Kurth, W. S., Labrianidis, C., Lainey, V., Lamy, L. L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J. I., Mousis, O., Nettelmann, N., Neubauer, F. M., Nordheim, T., Noyelles, B., Orton, G. S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C. T., Rymer, Am., Sallantin, R., Sanchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, Km., Schenk, P., Schubert, J., Sergis, N., Sittler, E. C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E. P., Vinatier, S., Wilson, R., Zarkat, P., Arridge, C. S., Achilleos, N., Agarwal, J., Agnor, C. B., Ambrosi, R., Andre, N., Badman, S. V., Baines, K., Banfield, D., Barthelemy, M., Bisi, M. M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B. ., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalie, T., Christophe, B., Coates, A. J., Collinson, G., Cooper, J. F., Costa-Sitja, M., Courtin, R., Daglis, I. A., De Pater, I., Desai, M., Dirkx, D., Dougherty, M. K., Ebert, R. W., Filacchione, G., Fletcher, L. N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grun, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J. K., Hofstadter, M. H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C. M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Kruger, H., Kurth, W. S., Labrianidis, C., Lainey, V., Lamy, L. L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J. I., Mousis, O., Nettelmann, N., Neubauer, F. M., Nordheim, T., Noyelles, B., Orton, G. S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C. T., Rymer, Am., Sallantin, R., Sanchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, Km., Schenk, P., Schubert, J., Sergis, N., Sittler, E. C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E. P., Vinatier, S., Wilson, R., and Zarkat, P.

Abstract

Giant planets helped to shape the conditions we see in the Solar System today and they account for more than 99% of the mass of the Sun's planetary system. They can be subdivided into the Ice Giants (Uranus and Neptune) and the Gas Giants (Jupiter and Saturn), which differ from each other in a number of fundamental ways. Uranus, in particular is the most challenging to our understanding of planetary formation and evolution, with its large obliquity, low self-luminosity, highly asymmetrical internal field, and puzzling internal structure. Uranus also has a rich planetary system consisting of a system of inner natural satellites and complex ring system, five major natural icy satellites, a system of irregular moons with varied dynamical histories, and a highly asymmetrical magnetosphere. Voyager 2 is the only spacecraft to have explored Uranus, with a flyby in 1986, and no mission is currently planned to this enigmatic system. However, a mission to the uranian system would open a new window on the origin and evolution of the Solar System and would provide crucial information on a wide variety of physicochemical processes in our Solar System. These have clear implications for understanding exoplanetary systems. In this paper we describe the science case for an orbital mission to Uranus with an atmospheric entry probe to sample the composition and atmospheric physics in Uranus' atmosphere. The characteristics of such an orbiter and a strawman scientific payload are described and we discuss the technical challenges for such a mission. This paper is based on a white paper submitted to the European Space Agency's call for science themes for its large-class mission programme in 2013. (C) 2014 Published by Elsevier Ltd.

Published
2014

23. The PHEMU09 catalogue and astrometric results of the observations of the mutual occultations and eclipses of the Galilean satellites of Jupiter made in 2009

Author

Arlot, J. -E., Emelyanov, N., Varfolomeev, M. I., Amossé, A., Arena, C., Assafin, M., Barbieri, L., Bolzoni, S., Bragas-Ribas, F., Camargo, J. I. B., Casarramona, F., Casas, R., Christou, A., Colas, F., Collard, A., Combe, S., Constantinescu, M., Dangl, G., De, Cat, P., Degenhardt, S., Delcroix, M., Dias-Oliveira, A., Dourneau, G., Douvris, A., Druon, C., Ellington, C. K., Estraviz, G., Farissier, P., Farmakopoulos, A., Garlitz, J., Gault, D., George, T., Gorda, S. Y., Grismore, J., Guo, D. F., Herald, D., Ida, M., Ishida, M., Ivanov, A. V., Klemt, B., Koshkin, N., Le, Campion, J. F., Liakos, A., Liao, S. L., Li, S. N., Loader, B., Lopresti, C., Lo, Savio, E., Marchini, A., Marino, G., Masi, G., Massallé, A., Maulella, R., Mcfarland, J., Miyashita, K., Napoli, C., Noyelles, B., Pauwels, T., Pavlov, H., Peng, Q. Y., Perelló, C., Priban, V., Prost, J., Razemon, S., Rousselle, J. P., Rovira, J., Ruisi, R., Ruocco, N., Salvaggio, F., Sbarufatti, G., Shakun, L., Scheck, A., Sciuto, C., Da, Silva, Neto, D. N., V, Sinyaeva, N., Sofia, A., Sonka, A., Talbot, J., Tang, Z. H., Tejfel, V. G., Thuillot, W., Tigani, K., Timerson, B., Tontodonati, E., Tsamis, V., Unwin, M., Venable, R., Vieira-Martins, R., Vilar, J., Vingerhoets, P., Watanabe, H., Yin, H. X., Yu, Y., Zambelli, R., Arlot, J. -E., Emelyanov, N., Varfolomeev, M. I., Amossé, A., Arena, C., Assafin, M., Barbieri, L., Bolzoni, S., Bragas-Ribas, F., Camargo, J. I. B., Casarramona, F., Casas, R., Christou, A., Colas, F., Collard, A., Combe, S., Constantinescu, M., Dangl, G., De, Cat, P., Degenhardt, S., Delcroix, M., Dias-Oliveira, A., Dourneau, G., Douvris, A., Druon, C., Ellington, C. K., Estraviz, G., Farissier, P., Farmakopoulos, A., Garlitz, J., Gault, D., George, T., Gorda, S. Y., Grismore, J., Guo, D. F., Herald, D., Ida, M., Ishida, M., Ivanov, A. V., Klemt, B., Koshkin, N., Le, Campion, J. F., Liakos, A., Liao, S. L., Li, S. N., Loader, B., Lopresti, C., Lo, Savio, E., Marchini, A., Marino, G., Masi, G., Massallé, A., Maulella, R., Mcfarland, J., Miyashita, K., Napoli, C., Noyelles, B., Pauwels, T., Pavlov, H., Peng, Q. Y., Perelló, C., Priban, V., Prost, J., Razemon, S., Rousselle, J. P., Rovira, J., Ruisi, R., Ruocco, N., Salvaggio, F., Sbarufatti, G., Shakun, L., Scheck, A., Sciuto, C., Da, Silva, Neto, D. N., V, Sinyaeva, N., Sofia, A., Sonka, A., Talbot, J., Tang, Z. H., Tejfel, V. G., Thuillot, W., Tigani, K., Timerson, B., Tontodonati, E., Tsamis, V., Unwin, M., Venable, R., Vieira-Martins, R., Vilar, J., Vingerhoets, P., Watanabe, H., Yin, H. X., Yu, Y., and Zambelli, R.

Abstract

Context. In 2009, the Sun and the Earth passed through the equatorial plane of Jupiter and therefore the orbital planes of its main satellites. It was the equinox on Jupiter. This occurrence made mutual occultations and eclipses between the satellites possible. Experience has shown that the observations of such events provide accurate astrometric data able to bring new information on the dynamics of the Galilean satellites. Observations are made under the form of photometric measurements, but need to be made through the organization of a worldwide observation campaign maximizing the number and the quality of the data obtained. Aims. This work focuses on processing the complete database of photometric observations of the mutual occultations and eclipses of the Galilean satellites of Jupiter made during the international campaign in 2009. The final goal is to derive new accurate astrometric data. Methods. We used an accurate photometric model of mutual events adequate with the accuracy of the observation. Our original method was applied to derive astrometric data from photometric observations of mutual occultations and eclipses of the Galilean satellites of Jupiter. Results. We processed the 457 lightcurves obtained during the international campaign of photometric observations of the Galilean satellites of Jupiter in 2009. Compared with the theory, for successful observations, the r.m.s. of O-C residuals are equal to 45.8 mas and 81.1 mas in right ascension and declination, respectively; the mean O-C residuals are equal to -2 mas and -9 mas in right ascension and declination, respectively, for mutual occultations; and -6 mas and +1 mas in right ascension and declination, respectively, for mutual eclipses. © ESO, 2014.

Published
2014

24. The science case for an orbital mission to Uranus:exploring the origins and evolution of ice giant planets

Author

Arridge, C. S., Achilleos, N., Agarwal, J., Agnor, C. B., Ambrosi, R., Andre, N., Badman, S. V., Baines, K., Banfield, D., Barthelemy, M., Bisi, M. M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B. ., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalie, T., Christophe, B., Coates, A. J., Collinson, G., Cooper, J. F., Costa-Sitja, M., Courtin, R., Daglis, I. A., De Pater, I., Desai, M., Dirkx, D., Dougherty, M. K., Ebert, R. W., Filacchione, G., Fletcher, L. N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grun, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J. K., Hofstadter, M. H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C. M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Kruger, H., Kurth, W. S., Labrianidis, C., Lainey, V., Lamy, L. L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J. I., Mousis, O., Nettelmann, N., Neubauer, F. M., Nordheim, T., Noyelles, B., Orton, G. S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C. T., Rymer, Am., Sallantin, R., Sanchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, Km., Schenk, P., Schubert, J., Sergis, N., Sittler, E. C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E. P., Vinatier, S., Wilson, R., Zarkat, P., Arridge, C. S., Achilleos, N., Agarwal, J., Agnor, C. B., Ambrosi, R., Andre, N., Badman, S. V., Baines, K., Banfield, D., Barthelemy, M., Bisi, M. M., Blum, J., Bocanegra-Bahamon, T., Bonfond, B. ., Bracken, C., Brandt, P., Briand, C., Briois, C., Brooks, S., Castillo-Rogez, J., Cavalie, T., Christophe, B., Coates, A. J., Collinson, G., Cooper, J. F., Costa-Sitja, M., Courtin, R., Daglis, I. A., De Pater, I., Desai, M., Dirkx, D., Dougherty, M. K., Ebert, R. W., Filacchione, G., Fletcher, L. N., Fortney, J., Gerth, I., Grassi, D., Grodent, D., Grun, E., Gustin, J., Hedman, M., Helled, R., Henri, P., Hess, S., Hillier, J. K., Hofstadter, M. H., Holme, R., Horanyi, M., Hospodarsky, G., Hsu, S., Irwin, P., Jackman, C. M., Karatekin, O., Kempf, S., Khalisi, E., Konstantinidis, K., Kruger, H., Kurth, W. S., Labrianidis, C., Lainey, V., Lamy, L. L., Laneuville, M., Lucchesi, D., Luntzer, A., MacArthur, J., Maier, A., Masters, A., McKenna-Lawlor, S., Melin, H., Milillo, A., Moragas-Klostermeyer, G., Morschhauser, A., Moses, J. I., Mousis, O., Nettelmann, N., Neubauer, F. M., Nordheim, T., Noyelles, B., Orton, G. S., Owens, M., Peron, R., Plainaki, C., Postberg, F., Rambaux, N., Retherford, K., Reynaud, S., Roussos, E., Russell, C. T., Rymer, Am., Sallantin, R., Sanchez-Lavega, A., Santolik, O., Saur, J., Sayanagi, Km., Schenk, P., Schubert, J., Sergis, N., Sittler, E. C., Smith, A., Spahn, F., Srama, R., Stallard, T., Sterken, V., Sternovsky, Z., Tiscareno, M., Tobie, G., Tosi, F., Trieloff, M., Turrini, D., Turtle, E. P., Vinatier, S., Wilson, R., and Zarkat, P.

Abstract

Giant planets helped to shape the conditions we see in the Solar System today and they account for more than 99% of the mass of the Sun's planetary system. They can be subdivided into the Ice Giants (Uranus and Neptune) and the Gas Giants (Jupiter and Saturn), which differ from each other in a number of fundamental ways. Uranus, in particular is the most challenging to our understanding of planetary formation and evolution, with its large obliquity, low self-luminosity, highly asymmetrical internal field, and puzzling internal structure. Uranus also has a rich planetary system consisting of a system of inner natural satellites and complex ring system, five major natural icy satellites, a system of irregular moons with varied dynamical histories, and a highly asymmetrical magnetosphere. Voyager 2 is the only spacecraft to have explored Uranus, with a flyby in 1986, and no mission is currently planned to this enigmatic system. However, a mission to the uranian system would open a new window on the origin and evolution of the Solar System and would provide crucial information on a wide variety of physicochemical processes in our Solar System. These have clear implications for understanding exoplanetary systems. In this paper we describe the science case for an orbital mission to Uranus with an atmospheric entry probe to sample the composition and atmospheric physics in Uranus' atmosphere. The characteristics of such an orbiter and a strawman scientific payload are described and we discuss the technical challenges for such a mission. This paper is based on a white paper submitted to the European Space Agency's call for science themes for its large-class mission programme in 2013. (C) 2014 Published by Elsevier Ltd.

Published
2014

25. The PHEMU09 catalogue and astrometric results of the observations of the mutual occultations and eclipses of the Galilean satellites of Jupiter made in 2009

Author

Arlot, J.-E., primary, Emelyanov, N., additional, Varfolomeev, M. I., additional, Amossé, A., additional, Arena, C., additional, Assafin, M., additional, Barbieri, L., additional, Bolzoni, S., additional, Bragas-Ribas, F., additional, Camargo, J. I. B., additional, Casarramona, F., additional, Casas, R., additional, Christou, A., additional, Colas, F., additional, Collard, A., additional, Combe, S., additional, Constantinescu, M., additional, Dangl, G., additional, De Cat, P., additional, Degenhardt, S., additional, Delcroix, M., additional, Dias-Oliveira, A., additional, Dourneau, G., additional, Douvris, A., additional, Druon, C., additional, Ellington, C. K., additional, Estraviz, G., additional, Farissier, P., additional, Farmakopoulos, A., additional, Garlitz, J., additional, Gault, D., additional, George, T., additional, Gorda, S. Yu., additional, Grismore, J., additional, Guo, D. F., additional, Herald, D., additional, Ida, M., additional, Ishida, M., additional, Ivanov, A. V., additional, Klemt, B., additional, Koshkin, N., additional, Le Campion, J. F., additional, Liakos, A., additional, Liao, S. L., additional, Li, S. N., additional, Loader, B., additional, Lopresti, C., additional, Lo Savio, E., additional, Marchini, A., additional, Marino, G., additional, Masi, G., additional, Massallé, A., additional, Maulella, R., additional, McFarland, J., additional, Miyashita, K., additional, Napoli, C., additional, Noyelles, B., additional, Pauwels, T., additional, Pavlov, H., additional, Peng, Q. Y., additional, Perelló, C., additional, Priban, V., additional, Prost, J., additional, Razemon, S., additional, Rousselle, J. P., additional, Rovira, J., additional, Ruisi, R., additional, Ruocco, N., additional, Salvaggio, F., additional, Sbarufatti, G., additional, Shakun, L., additional, Scheck, A., additional, Sciuto, C., additional, da Silva Neto, D. N., additional, V Sinyaeva, N., additional, Sofia, A., additional, Sonka, A., additional, Talbot, J., additional, Tang, Z. H., additional, Tejfel, V. G., additional, Thuillot, W., additional, Tigani, K., additional, Timerson, B., additional, Tontodonati, E., additional, Tsamis, V., additional, Unwin, M., additional, Venable, R., additional, Vieira-Martins, R., additional, Vilar, J., additional, Vingerhoets, P., additional, Watanabe, H., additional, Yin, H. X., additional, Yu, Y., additional, and Zambelli, R., additional

Published
2014
Full Text
View/download PDF

26. The PHEMU03 catalogue of observations of the mutual phenomena of the Galilean satellites of Jupiter

Author

Arlot, J. -E., Thuillot, W., Ruatti, C., Ahmad, A., Amosse, A., Anbazhagan, P., Andreyev, M., Antov, A., Appakutty, M., Asher, D., Aubry, S., Baron, N., Bassiere, N., Berthe, M., Bogdanovski, R., Bosq, F., Bredner, E., Buettner, D., Buromsky, M., Cammarata, S., Casas, R., Chis, G. D., Christou, A. A., Coquerel, J. -P., Corlan, R., Cremaschini, C., Crussaire, D., Cuypers, J., Dennefeld, M., Descamps, P., Devyatkin, A., Dimitrov, D., Dorokhova, T. N., Dorokhov, N. I., Dourneau, G., Duenas, M., Dumitrescu, A., Emelianov, N., Ferrara, D., Fiel, D., Fienga, A., Flatres, T., Foglia, S., Garlitz, J., Gerbos, J., Gilbert, R., Goncalves, R. M. D., Gonzales, D., Gorda, S. Yu., Gorshanov, D. L., Hansen, M. W., Harrington, M., Irsmambetova, T. R., Ito, Y., Ivanova, V., Izmailov, I. S., Khovritchev, M. Yu., Khrutskaya, E. V., Kieken, J., Kiseleva, T. P., Kuppuswamy, K., Lainey, V., Lavayssiere, M., Lazzarotti, P., Le Campion, J. -F., Lellouch, E., Li, Z. L., Lo Savio, E., Lou, M., Magny, E., Manek, J., Marinello, W., Marino, G., McAuliffe, J. P., Michelli, M., Moldovan, D., Montagnac, S., Moorthy, V., Nickel, O., Nier, J. M., Noel, T., Noyelles, B., Oksanen, A., Parrat, D., Pauwels, T., Peng, Q. Y., Pizzetti, G., Priban, V., Ramachandran, B., Rambaux, N., Rapaport, M., Rapavy, P., Rau, G., Sacre, J. -J., Sada, P. V., Salvaggio, F., Sarlin, P., Sciuto, C., Selvakumar, G., Sergeyev, A., Sidorov, M., Sorescu, S., Spampinato, S. A., Stellmacher, I., Trunkovsky, E., Tejfel, V., Tudose, V., Turcu, V., Ugarte, I., Vantyghem, P., Vasundhara, R., Vaubaillon, J., Velu, C., Venkataramana, A. K., Vidal-Sainz, J., Vienne, A., Vilar, J., Vingerhoets, P., Vollman, W., Arlot, J. -E., Thuillot, W., Ruatti, C., Ahmad, A., Amosse, A., Anbazhagan, P., Andreyev, M., Antov, A., Appakutty, M., Asher, D., Aubry, S., Baron, N., Bassiere, N., Berthe, M., Bogdanovski, R., Bosq, F., Bredner, E., Buettner, D., Buromsky, M., Cammarata, S., Casas, R., Chis, G. D., Christou, A. A., Coquerel, J. -P., Corlan, R., Cremaschini, C., Crussaire, D., Cuypers, J., Dennefeld, M., Descamps, P., Devyatkin, A., Dimitrov, D., Dorokhova, T. N., Dorokhov, N. I., Dourneau, G., Duenas, M., Dumitrescu, A., Emelianov, N., Ferrara, D., Fiel, D., Fienga, A., Flatres, T., Foglia, S., Garlitz, J., Gerbos, J., Gilbert, R., Goncalves, R. M. D., Gonzales, D., Gorda, S. Yu., Gorshanov, D. L., Hansen, M. W., Harrington, M., Irsmambetova, T. R., Ito, Y., Ivanova, V., Izmailov, I. S., Khovritchev, M. Yu., Khrutskaya, E. V., Kieken, J., Kiseleva, T. P., Kuppuswamy, K., Lainey, V., Lavayssiere, M., Lazzarotti, P., Le Campion, J. -F., Lellouch, E., Li, Z. L., Lo Savio, E., Lou, M., Magny, E., Manek, J., Marinello, W., Marino, G., McAuliffe, J. P., Michelli, M., Moldovan, D., Montagnac, S., Moorthy, V., Nickel, O., Nier, J. M., Noel, T., Noyelles, B., Oksanen, A., Parrat, D., Pauwels, T., Peng, Q. Y., Pizzetti, G., Priban, V., Ramachandran, B., Rambaux, N., Rapaport, M., Rapavy, P., Rau, G., Sacre, J. -J., Sada, P. V., Salvaggio, F., Sarlin, P., Sciuto, C., Selvakumar, G., Sergeyev, A., Sidorov, M., Sorescu, S., Spampinato, S. A., Stellmacher, I., Trunkovsky, E., Tejfel, V., Tudose, V., Turcu, V., Ugarte, I., Vantyghem, P., Vasundhara, R., Vaubaillon, J., Velu, C., Venkataramana, A. K., Vidal-Sainz, J., Vienne, A., Vilar, J., Vingerhoets, P., and Vollman, W.

Published
2009

30. The PHEMU03 catalogue of observations of the mutual phenomena of the Galilean satellites of Jupiter

Author

Arlot, J.-E., primary, Thuillot, W., additional, Ruatti, C., additional, Ahmad, A., additional, Amossé, A., additional, Anbazhagan, P., additional, Andreyev, M., additional, Antov, A., additional, Appakutty, M., additional, Asher, D., additional, Aubry, S., additional, Baron, N., additional, Bassiere, N., additional, Berthe, M., additional, Bogdanovski, R., additional, Bosq, F., additional, Bredner, E., additional, Buettner, D., additional, Buromsky, M., additional, Cammarata, S., additional, Casas, R., additional, Chis, G. D., additional, Christou, A. A., additional, Coquerel, J.-P., additional, Corlan, R., additional, Cremaschini, C., additional, Crussaire, D., additional, Cuypers, J., additional, Dennefeld, M., additional, Descamps, P., additional, Devyatkin, A., additional, Dimitrov, D., additional, Dorokhova, T. N., additional, Dorokhov, N. I., additional, Dourneau, G., additional, Dueñas, M., additional, Dumitrescu, A., additional, Emelianov, N., additional, Ferrara, D., additional, Fiel, D., additional, Fienga, A., additional, Flatres, T., additional, Foglia, S., additional, Garlitz, J., additional, Gerbos, J., additional, Gilbert, R., additional, Goncalves, R. M. D., additional, Gonzãles, D., additional, Gorda, S. Yu., additional, Gorshanov, D. L., additional, Hansen, M. W., additional, Harrington, M., additional, Irsmambetova, T. R., additional, Ito, Y., additional, Ivanova, V., additional, Izmailov, I. S., additional, Khovritchev, M. Yu., additional, Khrutskaya, E. V., additional, Kieken, J., additional, Kiseleva, T. P., additional, Kuppuswamy, K., additional, Lainey, V., additional, Lavayssiére, M., additional, Lazzarotti, P., additional, Le Campion, J.-F., additional, Lellouch, E., additional, Li, Z. L., additional, Lo Savio, E., additional, Lou, M., additional, Magny, E., additional, Manek, J., additional, Marinello, W., additional, Marino, G., additional, McAuliffe, J. P., additional, Michelli, M., additional, Moldovan, D., additional, Montagnac, S., additional, Moorthy, V., additional, Nickel, O., additional, Nier, J. M., additional, Noel, T., additional, Noyelles, B., additional, Oksanen, A., additional, Parrat, D., additional, Pauwels, T., additional, Peng, Q. Y., additional, Pizzetti, G., additional, Priban, V., additional, Ramachandran, B., additional, Rambaux, N., additional, Rapaport, M., additional, Rapavy, P., additional, Rau, G., additional, Sacré, J.-J., additional, Sada, P. V., additional, Salvaggio, F., additional, Sarlin, P., additional, Sciuto, C., additional, Selvakumar, G., additional, Sergeyev, A., additional, Sidorov, M., additional, Sorescu, S., additional, Spampinato, S. A., additional, Stellmacher, I., additional, Trunkovsky, E., additional, Tejfel, V., additional, Tudose, V., additional, Turcu, V., additional, Ugarte, I., additional, Vantyghem, P., additional, Vasundhara, R., additional, Vaubaillon, J., additional, Velu, C., additional, Venkataramana, A. K., additional, Vidal-Sãinz, J., additional, Vienne, A., additional, Vilar, J., additional, Vingerhoets, P., additional, and Vollman, W., additional

Published
2008
Full Text
View/download PDF

36. The PHEMU03 catalogue of observations of the mutual phenomena of the Galilean satellites of Jupiter

Author

Arlot, J.-E., Thuillot, W., Ruatti, C., Ahmad, A., Amoss?, A., Anbazhagan, P., Andreyev, M., Antov, A., Appakutty, M., Asher, D., Aubry, S., Baron, N., Bassiere, N., Berthe, M., Bogdanovski, R., Bosq, F., Bredner, E., Buettner, D., Buromsky, M., Cammarata, S., Casas, R., Chis, G., Christou, A., Coquerel, J.-P., Corlan, R., Cremaschini, C., Crussaire, D., Cuypers, J., Dennefeld, M., Descamps, P., Devyatkin, A., Dimitrov, D., Dorokhova, T., Dorokhov, N., Dourneau, G., Due?as, M., Dumitrescu, A., Emelianov, N., Ferrara, D., Fiel, D., Fienga, A., Flatres, T., Foglia, S., Garlitz, J., Gerbos, J., Gilbert, R., Goncalves, R., Gonz?les, D., Gorda, S., Gorshanov, D., Hansen, M., Harrington, M., Irsmambetova, T., Ito, Y., Ivanova, V., Izmailov, I., Khovritchev, M., Khrutskaya, E., Kieken, J., Kiseleva, T., Kuppuswamy, K., Lainey, V., Lavayssi?re, M., Lazzarotti, P., Le Campion, J.-F., Lellouch, E., Li, Z., Lo Savio, E., Lou, M., Magny, E., Manek, J., Marinello, W., Marino, G., McAuliffe, J., Michelli, M., Moldovan, D., Montagnac, S., Moorthy, V., Nickel, O., Nier, J., Noel, T., Noyelles, B., Oksanen, A., Parrat, D., Pauwels, T., Peng, Q., Pizzetti, G., Priban, V., Ramachandran, B., Rambaux, N., Rapaport, M., Rapavy, P., Rau, G., Sacr?, J.-J., Sada, P., Salvaggio, F., Sarlin, P., Sciuto, C., Selvakumar, G., Sergeyev, A., Sidorov, M., Sorescu, S., Spampinato, S., Stellmacher, I., Trunkovsky, E., Tejfel, V., Tudose, V., Turcu, V., Ugarte, I., Vantyghem, P., Vasundhara, R., Vaubaillon, J., Velu, C., Venkataramana, A., Vidal-S?inz, J., Vienne, A., Vilar, J., Vingerhoets, P., and Vollman, W.

Abstract

Context. In 2003, the Sun and the Earth passed through both the equatorial plane of Jupiter and therefore the orbital planes of its main satellites. Aims. During this period, mutual eclipses and occultations were observed and we present the data collected.Methods. Light curves of mutual eclipses and occultations were recorded by the observers of the international campaign PHEMU03 organized by the Institut de m?canique c?leste, Paris, France. Results. We completed 377?observations of 118?mutual events from 42?sites and the corresponding data are presented in this paper. For each observation, information about the telescope, receptor, site, and observational conditions are provided.Conclusions. This paper gathers all data and indicates a first estimate of its precision. This catalogue of these rare events should constitute an improved basis for accurate astrometric data useful in the development of dynamical models.

Published
2009

37. Titan's rotation

Author

Noyelles, B., Lema?tre, A., and Vienne, A.

Abstract

Aims.We study the forced rotation of Titan seen as a rigid body at the equilibrium Cassini state, involving the spin-orbit synchronization.Methods.We used both the analytical and the numerical ways. We analytically determined the equilibrium positions and the frequencies of the 3?free librations around it, while a numerical integration associated to frequency analysis gave us a more synthetic, complete theory, where the free solution split from the forced one. Results.We find a mean obliquity of 2.2 arcmin and the fundamental frequencies of the free librations of about 2.0977, 167.4883, and 306.3360?years. Moreover, we bring out the main role played by Titan's inclination on its rotation, and we suspect a likely resonance involving Titan's wobble.

Published
2008

38. Long-Term Evolution of the Saturnian System.

Author

Ćuk M, El Moutamid M, Lari G, Neveu M, Nimmo F, Noyelles B, Rhoden A, and Saillenfest M

Abstract

Here we present the current state of knowledge on the long-term evolution of Saturn's moon system due to tides within Saturn. First we provide some background on tidal evolution, orbital resonances and satellite tides. Then we address in detail some of the present and past orbital resonances between Saturn's moons (including the Enceladus-Dione and Titan-Hyperion resonances) and what they can tell us about the evolution of the system. We also present the current state of knowledge on the spin-axis dynamics of Saturn: we discuss arguments for a (past or current) secular resonance of Saturn's spin precession with planetary orbits, and explain the links of this resonance to the tidal evolution of Titan and a possible recent cataclysm in the Saturnian system. We also address how the moons' orbital evolution, including resonances, affects the evolution of their interiors. Finally, we summarize the state of knowledge about the Saturnian system's long-term evolution and discuss prospects for future progress., Competing Interests: Competing InterestsThe authors have no relevant financial or non-financial interests to disclose., (© The Author(s) 2024.)

Published
2024
Full Text
View/download PDF

39. Tilting Styx and Nix but not Uranus with a Spin-Precession-Mean-motion resonance.

Author

Quillen AC, Chen YY, Noyelles B, and Loane S

Abstract

A Hamiltonian model is constructed for the spin axis of a planet perturbed by a nearby planet with both planets in orbit about a star. We expand the planet-planet gravitational potential perturbation to first order in orbital inclinations and eccentricities, finding terms describing spin resonances involving the spin precession rate and the two planetary mean motions. Convergent planetary migration allows the spinning planet to be captured into spin resonance. With initial obliquity near zero, the spin resonance can lift the planet's obliquity to near 90 or 180 degrees depending upon whether the spin resonance is first or zero-th order in inclination. Past capture of Uranus into such a spin resonance could give an alternative non-collisional scenario accounting for Uranus's high obliquity. However we find that the time spent in spin resonance must be so long that this scenario cannot be responsible for Uranus's high obliquity. Our model can be used to study spin resonance in satellite systems. Our Hamiltonian model explains how Styx and Nix can be tilted to high obliquity via outward migration of Charon, a phenomenon previously seen in numerical simulations.

Published
2018
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results