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The current orbit of Atlas (SXV)

Published online by Cambridge University Press:  30 May 2022

Demétrio Tadeu Ceccatto Open the ORCID record for Demétrio Tadeu Ceccatto [Opens in a new window] ,
Nelson Callegari Jr.  and
Adrián Rodríguez
Demétrio Tadeu Ceccatto
Affiliation:
São Paulo State University (UNESP), Institute of Geosciences and Exact Sciences, Av 24-A 1515, 13506-900, Rio Claro, Brazil email: dt.ceccatto@unesp.br
Nelson Callegari Jr.
Affiliation:
São Paulo State University (UNESP), Institute of Geosciences and Exact Sciences, Av 24-A 1515, 13506-900, Rio Claro, Brazil email: dt.ceccatto@unesp.br
Adrián Rodríguez
Affiliation:
Observatório do Valongo, Universidade Federal do Rio de Janeiro, Ladeira do Pedro Antônio 43, 20080-090 Rio de Janeiro, Brazil
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Abstract

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With the success of the Cassini-Huygens mission, the dynamic complexity surrounding natural satellites of Saturn began to be elucidated. New ephemeris could be calculated with a higher level of precision, which made it possible to study in detail the resonant phenomena and, in particular, the 54:53 near mean-motion resonance between Prometheus and Atlas. For this task, we have mapped in details the domains of the resonance with dense sets of initial conditions and distinct ranges of parameters. Our initial goal was to identify possible regions in the phase space of Atlas for which some critical angles, associated with the 54:53 mean motion have a stable libration. Our investigations revealed that there is no possibility for the current Atlas orbital configuration to have any regular behavior since it is in a chaotic region located at the boundary of the 54:53 mean-motion resonance phase space. This result is in accordance with previous works (Cooper et al. 2015; Renner et al. 2016). In this work, we generalize such investigations by showing detailed aspects of the Atlas-Prometheus 54:53 mean-motion resonance, like the extension of the chaotic layers, the thin domain of the center of the 54:53 resonance, the proximity of other neighborhood resonances, among other secondary conclusions. In particular, we have also shown that even in the deep interior of the resonance, it is difficult to map periodic motion of the resonant pair for very long time spans.

Keywords

Resonant dynamicsmean-motiondynamical mapsAtlasPrometheusSaturn
Type
Research Article
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S364: Multi-scale (Time and Mass) Dynamics of Space Objects (Oct 2021) , October 2019 , pp. 120 - 127
Copyright
© The Author(s), 2022. Published by Cambridge University Press on behalf of International Astronomical Union

References

Callegari, N. Jr., Yokoyama, T. Numerical exploration of resonant dynamics in the system of Saturnian inner Satellites. Planetary and Space Science 58, 1906–1921 (2010).CrossRefGoogle Scholar
Callegari, N. Jr., Yokoyama, T. Dynamics of the 11:10 Corotation and Lindblad Resonances with Mimas, and Application to Anthe, Icarus, 348, 113820 (2020).CrossRefGoogle Scholar
Callegari, N. Jr., Rodrigues, A., Ceccatto, D. T. The current orbit of Methone (S/2004). Celest Mech Dyn Astr, accepted for publication (2021).CrossRefGoogle Scholar
Chambers, J. E. A hybrid sympletic integrator that permits close encounters betwwen massive bodies. Montly Notices of the Royal Astron. Society 304, 793–799 (1999).Google Scholar
Cooper, N. J. Renner, S. Murray, C. D., Evans, M. W. Saturn’s inner satellites orbits, and the chaotic motion of Atlas from new Cassini imaging observations. The Astronomical Journal 149, 27–45, (2015).CrossRefGoogle Scholar
El Moutamid, M. Renner, S. Sicardy, B. Coupling between corotation and Lindblad resonances in the elliptic planar three-body problem. Celest Mech Dyn Astr, 118, (2014).CrossRefGoogle Scholar
Everhart, E. An efficient integrator that uses Gauss-Radau spacings. In: IAU Coloquium 83, 185–202 (1985).Google Scholar
Greenberg, R. Apsidal Precession of Orbits about an Oblate Planet. The Astronomical Journal 86, 912–914 (1981).CrossRefGoogle Scholar
Murray, C. D, Dermott, S. F. Solar System Dynamics, Cambridge University Press (1999).Google Scholar
Peale, S. J. Origin and Evolution of the Natural Satellites. Annual Review of Astron. and Astrophys. 37, 533–602 (1999).CrossRefGoogle Scholar
Renner, S., Sicardy, B. Use of the Geometric Elements in Numerical Simulations. Celestial Mechanics and Dynamical Astronomy 94, 237–248 (2006).CrossRefGoogle Scholar
Renner, S. Cooper, J, N. El Moutmaid, M.; Sicardy, B. Vienne, A.; Morray, C. D. Sarlenfest, M. Origin of the chaotic motion of the Saturnian satellite Atlas. The Astronomical Journal, 151 (2016).Google Scholar
Spitale, J. N., Jacobson, R. A., Porco, C. C., Owen, W. M. Jr The Orbits of Saturn’s Small Satellites Derived from Combined Historic and Cassini Imaging Observations. The Astronomical Journal 132, 792–810 (2006).CrossRefGoogle Scholar
Thomas, P. C., Helfenstein, P. The small inner satellites of Saturn: Shapes, structures and some implications. Icarus 344, 113355 (2020).CrossRefGoogle Scholar