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138 results on '"Saturnian system"'

1. The orbit of Aegaeon and the 7:6 Mimas-Aegaeon resonance.

Author

Callegari Jr., Nelson and Rodríguez, Adrián

Abstract

Aegaeon (S/2008 S 1) is the last satellite discovered by the Cassini spacecraft at the end of the 2000 s. Like the satellites Methone and Anthe, it is involved in mean motion resonance with the mid-sized Mimas. In this work, we give a detailed analysis of the current orbit of Aegaeon identifying the resonant, secular and long-term perturbations due to Mimas and the oblateness of Saturn, and the effects of Tethys. For this task, we perform thousands of numerical simulations of full equations of motion of ensembles of small bodies representing clones of Aegaeon. We have mapped the domain of the 7:6 Mimas-Aegaeon resonance in the phase space of the semi-major axis and eccentricity. It displays a large area dominated by regular motions associated with the 7:6 corotation resonance surrounded by chaotic layers. Aegaeon is currently located very close to the periodic orbit of the resonance, which extends up to eccentricities ∼ 0.025 centered at semi-major axis ∼ 168 , 028 km. We show that the current orbit of Aegaeon has an important forced component in eccentricity due to the 7:6 resonance. The orbital inclination of Aegaeon has a non-negligible forced value due to long-term perturbations of Mimas. These two forced modes explain the complex perturbed orbit of Aegaeon without requiring the co-existence of multiple resonances. [ABSTRACT FROM AUTHOR]

Published
2023
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2. The current orbit of Methone (S/2004 S 1).

Author

Callegari Jr., Nelson, Rodríguez, Adrián, and Ceccatto, Demétrio Tadeu

Subjects
*EQUATIONS of motion, *MICROSPACECRAFT, *NUMERICAL integration, *RESONANCE, *CELESTIAL mechanics
Abstract

The Cassini spacecraft discovered many close-in small satellites in Saturnian system, and several of them exhibit exotic orbital states due to interactions with Mimas and the oblateness of the planet. This work is devoted to Methone, which is currently involved in a 15:14 mean-motion resonance with Mimas. We give an in-deep study on the current orbit of Methone by analyzing and identifying the short, resonant and long-term gravitational perturbations on its orbit. In addition, we perform numerical integrations of full equations of motion of ensembles of close-in small bodies orbiting the non-central field of Saturn. Spectral analyses of the orbits and interpretation of them in dynamical maps allow us to describe the orbit and the dynamics of Methone in view of resonant and long-term dynamics. We show that the current geometric orbit of Methone is aligned with Mimas' due to a forced resonant component in eccentricity, leading to simultaneous oscillations of several critical angles of the expanded disturbing function. Thus, we explain the simultaneous oscillations of four critical arguments associated to the resonance. The mapping of the Mimas–Methone resonance shows that the domains of the 15:14 Mimas–Methone resonance are dominated by regular motions associated to the Corotation resonance located at eccentricities lower than ∼ 0.015 and osculating semi-major axis in the interval 194,660–194,730 km. Methone is currently located deeply within this site. [ABSTRACT FROM AUTHOR]

Published
2021
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3. A Titan mission using the Direct Fusion Drive.

Author

Gajeri, Marco, Aime, Paolo, and Kezerashvili, Roman Ya.

Subjects
*THERMONUCLEAR fusion, *PROPELLANTS, *NUCLEAR reactions, *FUSION reactors, *LATENT heat of fusion, *DEUTERIUM, *ELECTRICAL energy, *PROPULSION systems
Abstract

The main purpose of this work is to perform an analysis of realistic new trajectories for a robotic mission to Saturn's largest moon, Titan, in order to demonstrate the great advantages related to the Direct Fusion Drive (DFD). The DFD is a D - 2 3 He fueled, aneutronic, thermonuclear fusion propulsion system (Cohen et al., 2019). This fusion propulsion concept is based on a magnetically confined field reversed configuration plasma, where the deuterium propellant is heated by fusion products, and then expanded into a magnetic nozzle, providing both thrust and electrical energy to the spacecraft. The trajectories calculations and analysis for the Titan mission are obtained based on the characteristics provided by the PPPL (Cohen et al., 2019) for a 2 MW-class DFD engine. Two different profile missions are considered: the first one is a thrust–coast–thrust profile with constant thrust and specific impulse, the second scenario is a continuous and constant thrust profile mission. Each mission study is divided into four different phases, starting from the initial low Earth orbit departure, the interplanetary trajectory, Saturn orbit insertion, and the Titan orbit insertion. For all mission phases, maneuver time and propellant consumption are calculated. The results of calculations and mission analysis offer a complete overview of the advantages in term of payload mass and travel time. It is important to emphasize that the deceleration capability is one of the DFD game changers: in fact, the DFD performance allows to rapidly reach high velocities and decelerate in even shorter time period. This capability results in a total trip duration of 2.6 years for the thrust–coast–thrust profile and less than 2 years for the continuous thrust profile. The high payload enabling capability, combined with the huge electrical power available from the fusion reactor leads to a tremendous advantage compared to present technology. • The Direct Fusion Drive (DFD) is based on the D-3He nuclear fusion reaction. • A thrust–coast–thrust profile for an Earth–Titan mission is studied. • A continuous thrust profile for an Earth–Titan mission is studied. • A total trip duration is 2.6 years for the thrust–coast–thrust profile mission. • A total trip duration is less than 2 years for the continuous thrust profile mission. [ABSTRACT FROM AUTHOR]

Published
2021
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4. Saturn

Author

Hall, James A., III, Beech, Martin, Series editor, and Hall III, James A.

Published
2016
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9. Icy Satellites: Geological Evolution and Surface Processes

Author

Jaumann, Ralf, Clark, Roger N., Nimmo, Francis, Hendrix, Amanda R., Buratti, Bonnie J., Denk, Tilmann, Moore, Jeffrey M., Schenk, Paul M., Ostro, Steve J., Srama, Ralf, Dougherty, Michele K., editor, Esposito, Larry W., editor, and Krimigis, Stamatios M., editor

Published
2009
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16. The current orbit of Methone (S/2004 S 1)

Author

Demétrio Tadeu Ceccatto, Adrián Rodríguez, N. Callegari, Universidade Estadual Paulista (UNESP), and Universidade Federal do Rio de Janeiro (UFRJ)

Subjects
Field (physics), media_common.quotation_subject, FOS: Physical sciences, Resonance (particle physics), Planet, Saturnian system, Saturn, Celestial mechanics, Dynamics of natural satellites, Eccentricity (behavior), Mathematical Physics, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Spacecraft, business.industry, Applied Mathematics, Astronomy, Equations of motion, Astronomy and Astrophysics, Computational Mathematics, Orbit, Space and Planetary Science, Modeling and Simulation, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Cassini spacecraft discovered many close-in small satellites in Saturnian system, and several of them exhibit exotic orbital states due to interactions with Mimas and the oblateness of the planet. This work is devoted to Methone, which is currently involved in a 15:14 Mean-Motion Resonance with Mimas. We give an in deep study the current orbit of Methone by analyzing and identifying the short, resonant and long-term gravitational perturbations on its orbit. In addition, we perform numerical integrations of full equations of motion of ensembles of close-in small bodies orbiting the non-central field of Saturn. Spectral analyses of the orbits and interpretation of them in dynamical maps allow us to describe the orbit and the dynamics of Methone in view of resonant and long-term dynamics. We show that the current geometric orbit of Methone is aligned with Mimas' due to a forced resonant component in eccentricity, leading to simultaneous oscillations of several critical angles of the expanded disturbing function. Thus, we explain the simultaneous oscillations of four critical arguments associated to the resonance. The mapping of the Mimas-Methone resonance shows that the domains of the 15:14 Mimas-Methone resonance are dominated by regular motions associated to the Corotation resonance located at eccentricities lower than $\sim 0.015$ and osculating semi-major axis in the interval 194,660-194,730 km. Methone is currently located deeply within this site., Published on Astronomy and Astrophysics

Published
2022

19. Are Saturn’s rings actually young?

Author

Hsiang-Wen Hsu, A. Crida, Sébastien Charnoz, and Luke Dones

Subjects
Solar System, History, 010504 meteorology & atmospheric sciences, Interpretation (philosophy), Rings of Saturn, Astronomy, Astronomy and Astrophysics, 01 natural sciences, Planet, Saturn, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Saturnian system
Abstract

Spectacular results from Cassini’s Grand Finale have provided constraints on the characteristics and evolutionary processes of Saturn’s rings. These results have been interpreted as proof that the rings are much younger than the Solar System, dramatically changing our view of the origin of the whole Saturnian system and attracting the attention of scientific media outlets. But we should keep in mind that the age of the rings has not actually been measured (which is impossible per se) but rather is inferred. Here, we put these latest results into perspective and we point out that the young-rings hypothesis has some unsolved problems. Other interpretations, compatible with rings as old as the Solar System, are still possible. Measurements from Cassini’s Grand Finale, when the spacecraft flew between Saturn and its rings, have been used to claim that the rings are much younger than the planet itself. However, this interpretation does not solve all of the inconsistencies, and the question of the age of Saturn’s rings is still open.

Published
2019
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20. Composition of Titan's Atmosphere

Author

Véronique Vuitton, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), David Alderton, and Scott A. Elias

Subjects
Solar System, Haze, 010504 meteorology & atmospheric sciences, Nitrogen, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], chemistry.chemical_element, 01 natural sciences, Methane, Astrobiology, Atmosphere, chemistry.chemical_compound, symbols.namesake, Saturn, Clouds, Saturnian system, 0103 physical sciences, Nitriles, 010303 astronomy & astrophysics, Aerosol, 0105 earth and related environmental sciences, Hydrocarbons, Dynamics, Pluto, Chemistry, chemistry, 13. Climate action, Huygens, symbols, Cassini, Titan (rocket family), Titan, Composition
Abstract

International audience; As a result of the 13-year exploration of the Saturn system by the Cassini-Huygens mission (2004–17), there has been a revolution in our understanding of Titan, Saturn's largest satellite. Titan's atmosphere shows the most complex chemistry in the solar system. A chain of chemical reactions is being initiated in the upper atmosphere by ionization and dissociation of the major species, nitrogen and methane, primarily by solar UV photons. The produced photochemical molecules and aerosols have a strong impact on the radiative budget of Titan's atmosphere, and hence on its temperature profile. Furthermore, transport by global dynamics, which reverses each half Titan year, greatly affects the distribution of these compounds. These complex couplings between chemistry, radiation, and dynamics make Titan's atmosphere an ideal laboratory to understand physical and chemical processes at play in atmospheres in general, particularly those showing the presence of photochemical haze such as Pluto or the increasing number of detected exoplanets showing hazy atmospheres. Finally, the study of Titan's chemistry has astrobiological implications as it naturally produces complex organic nitrogen species that settle to the surface to produce an organic soil. This material is postulated to be exposed to aqueous melt pools produced through meteoritic impact or cryovolcanism, or even to be transported to an underground ocean of liquid water. Therefore, we may entertain the idea that, in certain regions at the (sub-)surface of Titan, the results of chemistry leading to life as we know it may be present.

Published
2021
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22. Recent improvements of the Saturnian satellites atlases: Mimas, Enceladus, and Dione

Author

Roatsch, Th., Kersten, E., Hoffmeister, A., Wählisch, M., Matz, K.-D., and Porco, C.C.

Subjects
*SATURN (Planet), *MIMAS (Satellite), *ENCELADUS (Satellite), *DIONE (Satellite)
Abstract

Abstract: The Cassini Imaging Science Subsystem (ISS) acquired many high-resolution images (<1km/pixel) of the Icy Saturnian satellites during the nominal mission of the Cassini spacecraft between 2004 and 2008. These images were used to create high-resolution mosaics of these satellites. The Cassini mission is expected to continue till 2017 and high-resolution images of the first three years of the extension were used to improve the mosaics, especially in the Northern parts which were not illuminated during the nominal mission. These improved mosaics were the baseline for new versions of the atlases of Mimas, Enceladus, and Dione described in this paper. These new atlases supersede the previous versions from 2006 (Enceladus) and 2008 (Mimas and Dione), and include the official names of additional features, proposed by the Cassini imaging team, approved by the International Astronomical Union (IAU). The new atlases are available to the public through the Imaging Team''s website and the Planetary Data System (PDS). [Copyright &y& Elsevier]

Published
2013
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23. Giant impacts in the Saturnian system: A possible origin of diversity in the inner mid-sized satellites

Author

Sekine, Yasuhito and Genda, Hidenori

Subjects
*ASTRONOMICAL observations, *DISKS (Astrophysics), *SATELLITES of Saturn, *ASTRONOMICAL models, *ENERGY dissipation, *ROCKS, *COMPUTER simulation, *SOLAR system
Abstract

Abstract: It is widely accepted that Titan and the mid-sized regular satellites around Saturn were formed in the circum-Saturn disk. Thus, if these mid-sized satellites were simply accreted by collisions of similar ice-rock satellitesimals in the disk, the observed wide diversity in density (i.e., the rock fraction) of the Saturnian mid-sized satellites is enigmatic. A recent circumplanetary disk model suggests satellite growth in an actively supplied circumplanetary disk, in which Titan-sized satellites migrate inward by interaction with the gas and are eventually lost to the gas planet. Here we report numerical simulations of giant impacts between Titan-sized migrating satellites and smaller satellites in the inner region of the Saturnian disk. Our results suggest that in a giant impact with impact velocity ≥∼1.4 times the escape velocity and impact angle of ∼45°, a smaller satellite is destroyed, forming multiple mid-sized satellites with a very wide diversity in satellite density (the rock fraction=0–92wt%). Our results of the relationship between the mass and rock fraction of the satellites resulting from giant impacts reproduce the observations of the Saturnian mid-sized satellites. Giant impacts also lead to internal melting of the formed mid-sized satellites, which would initiate strong tidal dissipation and geological activity, such as those observed on Enceladus today and Tethys in the past. Our findings also imply that giant impacts might have affected the fundamental physical property of the Saturnian mid-sized satellites as well as those of the terrestrial planets in the solar system and beyond. [Copyright &y& Elsevier]

Published
2012
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24. High-resolution atlas of Rhea derived from Cassini-ISS images

Author

Roatsch, Th., Kersten, E., Wählisch, M., Hoffmeister, A., Matz, K.-D., Scholten, F., Wagner, R., Denk, T., Neukum, G., and Porco, C.C.

Subjects
*REMOTE-sensing images, *WEBSITES, *ATLASES, *SPACE telescopes
Abstract

Abstract: The Cassini Imaging Science Subsystem (ISS) acquired 370 high-resolution images (<500m/pixel) of Rhea during two close flybys and 9 non-targeted flybys between 2004 and 2010. We combined these images with lower-resolution Cassini images and others taken by the Voyager cameras to produce a high-resolution semi-controlled mosaic of Rhea. This global mosaic is the baseline for a high-resolution Rhea atlas. The nomenclature used in this atlas was proposed by the Cassini imaging team and approved by the International Astronomical Union (IAU). The atlas is available to the public through the Imaging Team''s website 〈http://ciclops.org/maps〉 and the Planetary Data System 〈http://pds.jpl.nasa.gov〉. This atlas completes the series of the atlases of the Saturnian medium-sized satellites Mimas, Enceladus, Tethys, Dione, Rhea, and Iapetus. [Copyright &y& Elsevier]

Published
2012
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25. TandEM: Titan and Enceladus mission.

Author

Coustenis, A., Atreya, S. K., Balint, T., Brown, R. H., Dougherty, M. K., Ferri, F., Fulchignoni, M., Gautier, D., Gowen, R. A., Griffith, C. A., Gurvits, L. I., Jaumann, R., Langevin, Y., Leese, M. R., Lunine, J. I., McKay, C. P., Moussas, X., Müller-Wodarg, I., Neubauer, F., and Owen, T. C.

Subjects
*ENCELADUS (Satellite), *TITAN (Satellite), *SPACE exploration, *SOLAR system, *SPACE vehicles, *ATMOSPHERE
Abstract

TandEM was proposed as an L-class (large) mission in response to ESA’s Cosmic Vision 2015–2025 Call, and accepted for further studies, with the goal of exploring Titan and Enceladus. The mission concept is to perform in situ investigations of two worlds tied together by location and properties, whose remarkable natures have been partly revealed by the ongoing Cassini–Huygens mission. These bodies still hold mysteries requiring a complete exploration using a variety of vehicles and instruments. TandEM is an ambitious mission because its targets are two of the most exciting and challenging bodies in the Solar System. It is designed to build on but exceed the scientific and technological accomplishments of the Cassini–Huygens mission, exploring Titan and Enceladus in ways that are not currently possible (full close-up and in situ coverage over long periods of time). In the current mission architecture, TandEM proposes to deliver two medium-sized spacecraft to the Saturnian system. One spacecraft would be an orbiter with a large host of instruments which would perform several Enceladus flybys and deliver penetrators to its surface before going into a dedicated orbit around Titan alone, while the other spacecraft would carry the Titan in situ investigation components, i.e. a hot-air balloon (Montgolfière) and possibly several landing probes to be delivered through the atmosphere. [ABSTRACT FROM AUTHOR]

Published
2009
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26. High-resolution Atlases of Mimas, Tethys, and Iapetus derived from Cassini-ISS images

Author

Roatsch, Th., Wählisch, M., Hoffmeister, A., Kersten, E., Matz, K.-D., Scholten, F., Wagner, R., Denk, T., Neukum, G., Helfenstein, P., and Porco, C.

Subjects
*ATLASES, *REMOTE-sensing images, *MIMAS (Satellite), *TETHYS (Satellite), *SATELLITES of Saturn, *SATURN (Planet)
Abstract

Abstract: The Cassini Imaging Science Subsystem (ISS) acquired 282, 258, and 513 high-resolution images (<800m/pixel) of Mimas, Tethys, and Iapetus, respectively, during two close flyby of Tethys and Iapetus and eight non-targeted flybys between 2004 and 2007. We combined these images with lower-resolution Cassini images and others taken by Voyager cameras to produce high-resolution semi-controlled mosaics of Mimas, Tethys, and Iapetus. These global mosaics are the baseline for high-resolution Mimas and Iapetus maps and a Tethys atlas. The nomenclature used in these maps was proposed by the Cassini imaging team and was approved by the International Astronomical Union (IAU). The two maps and the atlas are available to the public through the Imaging Team''s website [http://ciclops.org/maps] and the Planetary Data System [http://pds.jpl.nasa.gov]. [Copyright &y& Elsevier]

Published
2009
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27. High-resolution Dione atlas derived from Cassini-ISS images

Author

Roatsch, Th., Wählisch, M., Hoffmeister, A., Matz, K.-D., Scholten, F., Kersten, E., Wagner, R., Denk, T., Neukum, G., and Porco, C.

Subjects
*IMAGING systems in astronomy, *OPTICAL resolution, *DIONE (Satellite)
Abstract

Abstract: The Cassini imaging science subsystem (ISS) acquired 449 high-resolution images (<800m/pixel) during one close flyby of Dione in 2005 and three non-targeted flybys in 2004, 2006, and 2007. We combined these images with lower-resolution Cassini images and one other taken by Voyager cameras to produce a high-resolution semi-controlled mosaic of Dione. This global mosaic is the baseline for a high-resolution Dione atlas that consists of 15 tiles mapped at a scale of 1:1,000,000. The nomenclature used in this atlas was proposed by the Cassini imaging team and was approved by the International Astronomical Union (IAU). The whole atlas is available to the public through the Imaging Team''s website [http://ciclops.org/maps]. [Copyright &y& Elsevier]

Published
2008
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28. High-resolution Enceladus atlas derived from Cassini-ISS images

Author

Roatsch, Th., Wählisch, M., Giese, B., Hoffmeister, A., Matz, K.-D., Scholten, F., Kuhn, A., Wagner, R., Neukum, G., Helfenstein, P., and Porco, C.

Subjects
*PHOTOGRAPHIC equipment, *CAMERAS
Abstract

Abstract: The Cassini Imaging Science Subsystem (ISS) acquired 377 high-resolution images (<1km/pixel) during three close flybys of Enceladus in 2005 [Porco, C.C., et al., 2006. Cassini observes the active south pole of Enceladus. Science 311, 1393–1401.]. We combined these images with lower resolution Cassini images and four others taken by Voyager cameras to produce a high-resolution global controlled mosaic of Enceladus. This global mosaic is the baseline for a high-resolution Enceladus atlas that consists of 15 tiles mapped at a scale of 1:500,000. The nomenclature used in this atlas was proposed by the Cassini imaging team and was approved by the International Astronomical Union (IAU). The whole atlas is available to the public through the Imaging Team''s website (http://ciclops.org/maps). [Copyright &y& Elsevier]

Published
2008
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29. Mapping of the icy Saturnian satellites: First results from Cassini-ISS

Author

Roatsch, Th., Wählisch, M., Scholten, F., Hoffmeister, A., Matz, K.-D., Denk, T., Neukum, G., Thomas, P., Helfenstein, P., and Porco, C.

Subjects
*CAMERAS, *PHOTOGRAPHIC equipment, *SATELLITES of Saturn, *SOLAR system
Abstract

Abstract: Images of the icy Saturnian satellites Mimas, Enceladus, Tethys, Dione, Rhea, Iapetus, and Phoebe, derived by the Voyager and Cassini cameras are used to produce new local high-resolution image mosaics as well as global mosaics [http://ciclops.org, http://photojournal.jpl.nasa.gov]. These global mosaics are valuable both for scientific interpretation and for the planning of future flybys later in the ongoing Cassini orbital tour. Furthermore, these global mosaics can be extended to standard cartographic products. [Copyright &y& Elsevier]

Published
2006
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30. Cassini's geological and compositional view of Tethys

Author

Sebastien Rodriguez, Bernd Giese, Robert H. Brown, T. Roatsch, Roland Wagner, Cristina M. Dalle Ore, Dale P. Cruikshank, Kevin H. Baines, Phil D. Nicholson, Dennis L. Matson, Roger N. Clark, Bonnie J. Buratti, Fabrizio Capaccioni, Ralf Jaumann, Norbert Krupp, Katrin Stephan, Gianrico Filacchione, DLR Institute of Planetary Research, German Aerospace Center (DLR), Johannes Kepler Universität Linz - Johannes Kepler University Linz [Autriche] (JKU), NASA Ames Research Center (ARC), University of Arizona, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, ITA, USA, FRA, and DEU

Subjects
Eismonde Tethys Cassini Mission, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Spectral properties, Astronomy and Astrophysics, Spatial distribution, 01 natural sciences, Saturnian satellite, Astrobiology, Graben, Paleontology, Space and Planetary Science, Saturn, 0103 physical sciences, Satellite, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Geology, 0105 earth and related environmental sciences, Saturnian system
Abstract

The Saturnian satellite Tethys exhibits geological and spectral properties, whose appearance, nature and spatial distribution partly mirror those identified on the neighboring satellites Dione and Rhea or fit to the picture how spectral surface properties are expected to change from one satellite to the other within the inner Saturnian system. However, we also identified spectral variations that are unique in the Saturnian system. Whereas geologically young surface features are characterized by pure H2O-ice composition with relatively large particles, which match the particle sizes measured for fresh surface features also on Dione and Rhea, geologically old weathered regions are dominated by submicron-sized ice particles. Our investigations confirm that the Odysseus impact event did not cause the formation of Tethys' extended graben system Ithaca Chasma. On the contrary, Odysseus might be responsible for the N-S trending 'icy' bands that mark Tethys' surface in the center of its leading and trailing hemisphere.

Published
2016
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33. The genesis of Cassini-Huygens

Author

Daniel Gautier, Tobias Owen, and Wing Ip

Subjects
symbols.namesake, Solar System, Civilization, Planetary science, media_common.quotation_subject, Humanity, symbols, Glory, Titan (rocket family), Space exploration, Saturnian system, Astrobiology, media_common
Abstract

1 Introduction: Titan viewed from Earth The reasonable man adapts himself to the world; the unreasonable one persists in trying to adapt the world to himself. Therefore all progress depends on the unreasonable man . - George Bernard Shaw The exploration of the solar system has become an important part of the glory and dreams of our civilization. The study of the Saturnian system and Titan itself can be traced back more than 400 years to when Galileo first pointed his telescope to the night sky to seek the mysteries of the universe. The Cassini-Huygens mission represents the first time in human history that a spacecraft was sent to spend time in the Saturnian system for close-up observations, bringing humanity to the surface of one of Saturn's satellites. We believe that this extraordinary achievement will be remembered as a major milestone in planetary exploration 400 years from now. More than that, it is also the first planetary science project of truly global scale, with scientists from three continents joining the effort. How did it come about? To begin, let us first summarize what we knew about Titan before the birth of the Cassini-Huygens mission. Comprehensive descriptions of Titan studies during the period from its discovery in 1655 to the landing of the Huygens probe in 2001 have been published by Fortes (1997) and Coustenis et al. (2009). Here we simply present a few highlights in chronological order.

Published
2014
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34. The influence of imperfect accretion and radial mixing on ice:rock ratios in the Galilean satellites

Author

Shigeru Ida, C. A. Dwyer, Masahiro Ogihara, and Francis Nimmo

Subjects
Accretion (meteorology), Astronomy, Astronomy and Astrophysics, Geophysics, Galilean moons, Satellite diversity, symbols.namesake, Space and Planetary Science, Erosion, symbols, Satellite, Astrophysics::Earth and Planetary Astrophysics, Imperfect, Physics::Atmospheric and Oceanic Physics, Geology, Mixing (physics), Saturnian system
Abstract

We investigate the origin of the steep compositional gradient inferred for the Galilean satellites. We analyze N-body simulations of satellite accretion (Ogihara, M., Ida, S. [2012]. Astrophys. J. 753, 60) to: (1) determine the extent to which individual satellites accrete material from different semi-major axes (‘radial mixing’); and (2) calculate the change in rock:ice ratios due to vapor production or physical erosion during collisions. Because of inwards migration, satellites experience enough radial mixing that any initial compositional gradient is efficiently smoothed out. Mean-motion resonances generally prevent large proto-satellites from colliding with each other; as a result, neither vapor production nor physical erosion are capable of explaining the steep compositional gradient. According to the models presented here, even combining an initial compositional gradient with impact-related mass loss cannot reproduce the observed gradient. Some other physical process must have been responsible, perhaps tidally-driven volatile loss at Io and Europa. Impact-related mass loss was probably more important in the saturnian system, and may explain some of the observed satellite diversity there.

Published
2013
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36. Searching for Saturn’s dust swarm: limits on the size distribution of irregular satellites from km to micron sizes

Author

Grant M. Kennedy, John Stansberry, Kate Y. L. Su, and Mark C. Wyatt

Subjects
Solar System, Swarm behaviour, Astronomy and Astrophysics, Scale (descriptive set theory), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Distribution (mathematics), Space and Planetary Science, Asteroid, Saturn, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Satellite, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Geology, Saturnian system
Abstract

We describe a search for dust created in collisions between the Saturnian irregular satellites using archival \emph{Spitzer} MIPS observations. Although we detected a degree scale Saturn-centric excess that might be attributed to an irregular satellite dust cloud, we attribute it to the far-field wings of the PSF due to nearby Saturn. The Spitzer PSF is poorly characterised at such radial distances, and we expect PSF characterisation to be the main issue for future observations that aim to detect such dust. The observations place an upper limit on the level of dust in the outer reaches of the Saturnian system, and constrain how the size distribution extrapolates from the smallest known (few km) size irregulars down to micron-size dust. Because the size distribution is indicative of the strength properties of irregulars, we show how our derived upper limit implies irregular satellite strengths more akin to comets than asteroids. This conclusion is consistent with their presumed capture from the outer regions of the Solar System.

Published
2011
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37. Probing the origin of the dark material on Iapetus

Author

Diego Turrini, Federico Tosi, Gianrico Filacchione, Angioletta Coradini, and Vims Team

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, Saturn, Near-infrared spectroscopy, Imaging spectrometer, FOS: Physical sciences, High resolution, Astronomy, Astronomy and Astrophysics, Satellite, Geology, Astrophysics - Earth and Planetary Astrophysics, Saturnian system
Abstract

Among the icy satellites of Saturn, Iapetus shows a striking dichotomy between its leading and trailing hemispheres, the former being significantly darker than the latter. Thanks to the VIMS imaging spectrometer on-board Cassini, it is now possible to investigate the spectral features of the satellites in Saturn system within a wider spectral range and with an enhanced accuracy than with previously available data. In this work, we present an application of the G-mode method to the high resolution, visible and near infrared data of Phoebe, Iapetus and Hyperion collected by Cassini/VIMS, to search for compositional correlations. We also present the results of a dynamical study on the efficiency of Iapetus in capturing dust grains travelling inward in Saturn system to evaluate the viability of Poynting-Robertson drag as the physical mechanism transferring the dark material to the satellite. The results of spectroscopic classification are used jointly with the ones of the dynamical study to describe a plausible physical scenario for the origin of Iapetus' dichotomy. Our work shows that mass transfer from the outer Saturnian system is an efficient mechanism, particularly for the range of sizes hypothesised for the particles composing the newly discovered outer ring around Saturn. Both spectral and dynamical data indicate Phoebe as the main source of the dark material. However, we suggest a multi-source scenario where now extinct prograde satellites and the disruptive impacts that generated the putative collisional families played a significant role in supplying the original amount of dark material., Comment: 20 pages, 4 tables, 11 figures, major revision (manuscript extended and completed, figures added and corrected, new results added), minor revision and finalization of author list, moderate revision (update of the manuscript following reviewer's feedback and discovery of the new Saturnian outer ring)

Published
2010
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38. Astrometric studies of the series of photographic and CCD observations of the Saturnian system with the 26-inch Pulkovo refractor in 1995-2007

Author

T. A. Vasilieva, I. S. Izmailov, O. A. Kalinichenko, and T. P. Kiseleva

Subjects
Physics, Photographic plate, Series (mathematics), Space and Planetary Science, Saturn, Refracting telescope, Astronomy and Astrophysics, Satellite, Right ascension, Geodesy, Declination, Saturnian system, Remote sensing
Abstract

The results of the reduction, investigation, and comparison of the photographic observations of the major Saturnian satellites and CCD observations with an ST6 CCD camera obtained at the 264nch Pulkovo refractor in 1995–2007 are presented. A comparison of the observational results with the TASS 1.7 theory of motion of the Saturnian satellites has served as the basis for investigating and comparing the series of observations. The period-averaged (O-C) residuals and observational errors have been calculated. A comparison of the series of CCD and photographic observations has shown the same external accuracy of the observations at a higher internal accuracy of the CCD observations than that of the photographic ones. A comparison of the Pulkovo results with those of other authors has shown them to be close in accuracy. The accuracy of the theory has been estimated by comparing simultaneous (on the same night) CCD and photographic observations. The errors of the observations and the theory have been found from this comparison to be the following: 0.081“ and 0.067” for the observations and 0.077“ and 0.115” for the theory (inxandy, respectively). An analysis of the dependence of (O-C)x,y for three satellites (the sixth, seventh, and eighth) on the satellite positions in Saturn-centered orbits has revealed systemat ic deviations for the seventh satellite in both coordinates. The positions of Saturn have been determined from satellite observations without measuring its images on photographic plates with accuracies of 0.121“ and 0.105” in right ascension and declination, respectively.

Published
2010
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39. TandEM: Titan and Enceladus mission

Author

J. E. Blamont, Tobias Owen, Michael Küppers, Xenophon Moussas, Robert H. Brown, Nicole Schmitz, Sascha Kempf, C. Menor Salvan, T. W. Haltigin, Olivier Grasset, Roger V. Yelle, Wayne H. Pollard, Daniel Gautier, Paul R. Mahaffy, Joe Pitman, Iannis Dandouras, Daphne Stam, John C. Zarnecki, Bruno Sicardy, Georges Durry, Jesús Martínez-Frías, Norbert Krupp, S. Le Mouélic, Matthias Grott, Sébastien Lebonnois, T. Krimigis, Elizabeth P. Turtle, Alain Herique, Linda Spilker, Ralph D. Lorenz, Maria Teresa Capria, M. Combes, John F. Cooper, O. Mousis, Joachim Saur, Wlodek Kofman, J. Bouman, M. Paetzold, Hojatollah Vali, C. Dunford, Sushil K. Atreya, Eric Chassefière, I. de Pater, T. B. McCord, Bruno Bézard, Gabriel Tobie, Catherine D. Neish, M. Ruiz Bermejo, Sergei Pogrebenko, Kim Reh, Athena Coustenis, Ralf Jaumann, Angioletta Coradini, Leonid I. Gurvits, Andrew J. Coates, Tibor S. Balint, H. Hussmann, E. Choi, Ioannis A. Daglis, Edward C. Sittler, Emmanuel Lellouch, Robert A. West, L. Boireau, E.F. Young, Timothy A. Livengood, Cesar Bertucci, Martin G. Tomasko, M. Fujimoto, Ingo Müller-Wodarg, Yves Bénilan, Wing-Huen Ip, Marina Galand, Darrell F. Strobel, Cyril Szopa, Pascal Rannou, D. G. Mitchell, Mark Leese, Véronique Vuitton, P. Annan, Tetsuya Tokano, Caitlin A. Griffith, Conor A. Nixon, Stephen A. Ledvina, Karoly Szego, Andrew Morse, Panayotis Lavvas, Luisa Lara, C. de Bergh, Jonathan I. Lunine, R. A. Gowen, Katrin Stephan, Jianping Li, Glenn S. Orton, Michel Blanc, Esa Kallio, Ronan Modolo, M. Hirtzig, Helmut Lammer, Nicholas Achilleos, D. Nna Mvondo, Frank Sohl, M. Nakamura, Andrew Steele, C. C. Porco, Marcello Fulchignoni, Gordon L. Bjoraker, Olga Prieto-Ballesteros, J. J. López-Moreno, Andrew Dominic Fortes, Rafael Rodrigo, Patrice Coll, Francesca Ferri, François Raulin, Tom Spilker, F. J. Crary, J. H. Waite, Dirk Schulze-Makuch, Thomas E. Cravens, Kevin H. Baines, C. P. McKay, L. Richter, D. Luz, David H. Atkinson, Martin Knapmeyer, Robert E. Johnson, D. Fairbrother, F. M. Flasar, Roland Thissen, Paul N. Romani, Sebastien Rodriguez, Urs Mall, Paul M. Schenk, Franck Hersant, R. Koop, Odile Dutuit, I. Vardavas, T. Kostiuk, Ricardo Amils, Konrad Schwingenschuh, Robert V. Frampton, Fritz M. Neubauer, Jan-Erik Wahlund, L. A. Soderblom, Michele K. Dougherty, Anna Milillo, Frank T. Robb, Bernard Schmitt, Christophe Sotin, Michel Cabane, A. Selig, Bernard Marty, Yves Langevin, Rosaly M. C. Lopes, Emmanuel T. Sarris, E. De Angelis, D. Toublanc, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Space and Atmospheric Physics Group [London], Blackett Laboratory, Imperial College London-Imperial College London, Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Università degli Studi di Padova = University of Padua (Unipd), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Joint Institute for VLBI in Europe (JIVE ERIC), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), The Open University [Milton Keynes] (OU), NASA Ames Research Center (ARC), Department of Physics [Athens], National and Kapodistrian University of Athens (NKUA), University of Cologne, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Swedish Institute of Space Physics [Uppsala] (IRF), Space Science Division [San Antonio], Southwest Research Institute [San Antonio] (SwRI), Centre National d'Études Spatiales [Toulouse] (CNES), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Academy of Athens, Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Space Science Institute [Boulder] (SSI), Bombardier Aerospace, Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Sensors and Software, University of Idaho [Moscow, USA], SRON Netherlands Institute for Space Research (SRON), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Istituto Nazionale di Astrofisica (INAF), University of Kansas [Lawrence] (KU), National Observatory of Athens (NOA), Department of Astronomy [Berkeley], University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie de Grenoble (LPG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), McGill University = Université McGill [Montréal, Canada], FORMATION STELLAIRE 2009, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), University of Virginia [Charlottesville], Finnish Meteorological Institute (FMI), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratory of Numerical Modeling for Atmospheric Sciences and Geophysical Fluid Dynamics (LASG), Institute of Atmospheric Physics [Beijing] (IAP), Chinese Academy of Sciences [Beijing] (CAS)-Chinese Academy of Sciences [Beijing] (CAS), National Center for Earth and Space Science Education (NCESSE), Observatório Astronómico de Lisboa, Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Bear Fight Center, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Lockheed Martin Space, Groupe de spectrométrie moléculaire et atmosphérique (GSMA), Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), University of Maryland Biotechnology Institute Baltimore, University of Maryland [Baltimore], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Democritus University of Thrace (DUTH), Lunar and Planetary Institute [Houston] (LPI), School of Earth and Environmental Sciences [Pullman], Washington State University (WSU), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universita degli Studi di Padova, National and Kapodistrian University of Athens = University of Athens (NKUA | UoA), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), IMPEC - LATMOS, University of California [Berkeley], University of California-University of California, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), McGill University, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), University of Virginia, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
Exploration of Saturn, Solar System, Cosmic Vision, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Computer science, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], TandEM, 01 natural sciences, law.invention, Astrobiology, Enceladus, Orbiter, symbols.namesake, law, Saturnian system, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Spacecraft, Tandem, business.industry, Astronomy and Astrophysics, Landing probes, Space and Planetary Science, symbols, Titan, business, Titan (rocket family)
Abstract

著者人数：156名, Accepted: 2008-05-27, 資料番号: SA1000998000

Published
2009
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40. The phase curve survey of the irregular saturnian satellites: A possible method of physical classification

Author

Bonnie J. Buratti, James M. Bauer, Michael D. Hicks, and T. Grav

Subjects
Physics, Brightness, Solar System, Phase (waves), Astronomy, Astronomy and Astrophysics, Phase curve, law.invention, Telescope, Space and Planetary Science, Observatory, law, Surge, Saturnian system
Abstract

During its 2005 January opposition, the saturnian system could be viewed at an unusually low phase angle. We surveyed a subset of Saturn's irregular satellites to obtain their true opposition magnitudes, or nearly so, down to phase angle values of 0.01 deg. Combining our data taken at the Palomar 200-inch and Cerro Tololo Inter-American Observatory's 4-m Blanco telescope with those in the literature, we present the first phase curves for nearly half the irregular satellites originally reported by Gladman et al. [2001. Nature 412, 163-166], including Paaliaq (SXX), Siarnaq (SXXIX), Tarvos (SXXI), Ijiraq (SXXII), Albiorix (SXVI), and additionally Phoebe's narrowest angle brightness measured to date. We find centaur-like steepness in the phase curves or opposition surges in most cases with the notable exception of three, Albiorix and Tarvos, which are suspected to be of similar origin based on dynamical arguments, and Siarnaq.During its 2005 January opposition, the saturnian system could be viewed at an unusually low phase angle. We surveyed a subset of Saturn's irregular satellites to obtain their true opposition magnitudes, or nearly so, down to phase angle values of 0.01 deg. Combining our data taken at the Palomar 200-inch and Cerro Tololo Inter-American Observatory's 4-m Blanco telescope with those in the literature, we present the first phase curves for nearly half the irregular satellites originally reported by Gladman et al. [2001. Nature 412, 163-166], including Paaliaq (SXX), Siarnaq (SXXIX), Tarvos (SXXI), Ijiraq (SXXII), Albiorix (SXVI), and additionally Phoebe's narrowest angle brightness measured to date. We find centaur-like steepness in the phase curves or opposition surges in most cases with the notable exception of three, Albiorix and Tarvos, which are suspected to be of similar origin based on dynamical arguments, and Siarnaq.

Published
2006
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41. Analysing the New Saturnian Rings, R/2004 S1 and R/2004 S2

Author

S. M. Giuliatti Winter, D. C. Mourão, T. A. Bastos, and Rafael Sfair

Subjects
Physics, Mathematics::Commutative Algebra, Atlas (topology), Astronomy and Astrophysics, Lyapunov exponent, Astrophysics, Ring (chemistry), symbols.namesake, Space and Planetary Science, Physics::Space Physics, Earth and Planetary Sciences (miscellaneous), symbols, Satellite, Atomic physics, Saturnian system, Planetary ring
Abstract

The Cassini-Huygens arrival into the Saturnian system brought a large amount of data about the satellites and rings. Two diffuse rings were found in the region between the A ring and Prometheus. R/2004 S1 is coorbital to Atlas and R/2004 S2 is close to Prometheus. In this work we analysed the closest approach between Prometheus and both rings. As a result we found that the satellite removes particles from R/2004 S2 ring. Long-term numerical simulations showed that some particles can cross the F ring region . The well known region of the F ring, where small satellites are present and particles are being taking from the ring, gains a new insight with the presence of particles from R/2004 S2 ring. The computation of the Lyapunov Characteristic Exponent reveled that the R/2004 S2 ring lies in a chaotic region while R/2004 S1 ring and Atlas are in a stable region. Atlas is responsible for the formation of three regimes in the R/2004 S1 ring, as expected for a satellite embedded in a ring.

Published
2006
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42. Cassini/Huygens at Saturn and Titan

Author

Robert T. Mitchell

Subjects
Exploration of Saturn, Atmospheric sounding, Physics, Spacecraft, business.industry, Aerospace Engineering, Flight time, Astrobiology, law.invention, Orbiter, symbols.namesake, law, symbols, business, Interplanetary spaceflight, Titan (rocket family), Geology, Saturnian system
Abstract

The Cassin/Huygens Project is a joint undertaking between NASA, the European Space Agency, and the Italian Space Agency to conduct an in-depth exploration of the Saturnian system. The spacecraft consists of an orbiter vehicle and an atmospheric probe which has completed its mission in the atmosphere and on the surface of Titan, the largest moon of Saturn. The spacecraft was launched on October 15, 1997, has completed its nearly seven years of interplanetary flight, and by the time of the 56th IAC, it will have completed 17 of its planned 75 orbits during its four-year prime orbital mission. This paper gives an overview of the mission, and describes in detail the accomplishments and events over the past year, including the spectacularly successful descent of the .European Space Agency's Huygens probe to the surface of Titan. Initial scientific results from both the Huygens mission as well as from the first one-and-a-quarter years of orbiting Saturn are summarized. The plans for the remainder of the orbiter's tour of the Saturn system and the many flybys of Titan and the smaller icy satellites are described.

Published
2006
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43. THE CASSINI / HUYGENS SPACE MISSION TO EXPLORE THE SATURNIAN SYSTEM

Author

Klaus Schilling

Subjects
Exploration of Saturn, Spacecraft, Failure diagnosis, business.industry, General Medicine, Astrobiology, symbols.namesake, Geography, Planet, Mission analysis, symbols, Interplanetary spacecraft, business, Titan (rocket family), Saturnian system
Abstract

The Cassini/Huygens spacecraft arrived in July 2004 at the planet Saturn and landed on 14. January 2005 the atmospheric descent probe Huygens successfully on the surface of Titan, Saturn's largest moon. This paper reviews the related technical challenges and the solutions with emphasis on control engineering aspects. Addressed is the design of a trajectory to bring a spacecraft of almost 6 t by gravity assisted fly-bys to Saturn, despite this is beyond the direct capacity of available launchers. Remote failure diagnosis is highlighted at the example of the telecommunication link problem detected at the distance of Jupiter. In the course of the 10 years long development process different approaches to the descent control system had been discussed for the Huygens probe to enable a safe landing on Titan, satisfying given schedule constraints. These approaches will be compared and discussed in relation to the finally realized solution.

Published
2005
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44. The Orbits of the Major Saturnian Satellites and the Gravity Field of Saturn from Spacecraft and Earth-based Observations

Author

Robert A. Jacobson

Subjects
Physics, Gravity (chemistry), Spacecraft, business.industry, Astronomy, Astronomy and Astrophysics, Saturnian, Ephemeris, Gravitational field, Space and Planetary Science, Saturn, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, Physics::Atmospheric and Oceanic Physics, Saturnian system
Abstract

We have fitted numerically integrated orbits for the major Saturnian satellites to a large set of astrometric observations over the time interval 1966 September to 2003 December and to data obtained with the Pioneer 11, Voyager, and Cassini spacecraft. The results of the fit are new ephemerides for the satellites and a revised gravity field for the Saturnian system. We include an accuracy assessment for the ephemerides and the gravity parameters.

Published
2004
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45. New perspectives on Titan's upper atmosphere from a reanalysis of the Voyager 1 UVS solar occultations

Author

Bill R. Sandel, Darrell F. Strobel, and Ronald J. Vervack

Subjects
Atmosphere, Solar System, symbols.namesake, Space and Planetary Science, Aeronomy, symbols, Astronomy, Environmental science, Astronomy and Astrophysics, Titan (rocket family), Occultation, Data reduction, Saturnian system
Abstract

We have reanalyzed the Voyager 1 UVS solar occultations by Titan to expand upon previous analyses and to resolve inconsistencies that have been noted in the scientific literature. To do so, we have developed a detailed model of the UVS detector and improved both the data reduction methods and retrieval techniques. In comparison to the values previously determined by Smith et al. (1982, J. Geophys. Res. 87, 1351–1359) we find N2 densities that are 25–60% higher, CH4 densities that are smaller by a factor of 3–7, and C2H2 densities that are roughly two orders of magnitude smaller. Our values for the thermospheric temperature are 153–158 K, which are approximately 20–40 K colder than previous estimates. We also report the first-ever determination from Voyager UVS data of density profile information for C2H4, HCN, and HC3N. Finally, we present a simple engineering model that is consistent with our new results in the upper atmosphere and merges smoothly with the model of Yelle et al. (1997, in: HUYGENS Science, Payload and Mission, in: ESA SP, vol. 1177, pp. 243–256) in the lower atmosphere. Our results provide improved constraints for photochemical models and offer scientists a better understanding of Titan's upper atmosphere as we head into the Cassini era in the exploration of the saturnian system.

Published
2004
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46. Observing the South Pole of Enceladus using Cassini/CIRS as a Radiometer

Author

Nicolas Gorius

Subjects
Geography, Radiometer, Spectrometer, Spacecraft, business.industry, Radiometry, Enceladus, business, Astrobiology, Remote sensing, Saturnian system
Abstract

The Composite Infrared Spectrometer aboard the Cassini spacecraft has been making numerous observations of the Saturnian system since 2004. This talk will present the instrument models specifically developed to analyze our observations of the South Pole of Enceladus while using CIRS as a radiometer.

Published
2015
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48. HUYGENS ATMOSPHERIC STRUCTURE INSTRUMENT OF HUYGENS PROBE ON CASSINI MISSION

Author

Francesca Ferri, Francesco Angrilli, G. Bianchini, M. Fulchignoni, and Hasi Team

Subjects
Physics, symbols.namesake, symbols, Aerospace Engineering, Electric properties, Atmosphere of Titan, Titan (rocket family), Remote sensing, Saturnian system, Physical quantity
Abstract

In the framework of the Cassini-Huygens mission towards the Saturnian system, the Huygens Atmospheric Structure Instrument (HASI) is a multisensor package which has been designed to measure the physical quantities characterizing the atmosphere of Titan, Saturn's largest satellite. HASI sensors are devoted to the study of Titan's atmospheric structure and electric properties, and also to provide information on the surface, whatever its phase, solid or liquid. A description of the experiment, its subsystems and sensors package is reported together with their performances.

Published
2002
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49. [Untitled]

Author

Aron A. Wolf

Subjects
business.industry, Computer science, Astronomy and Astrophysics, law.invention, Astrobiology, Orbiter, symbols.namesake, Design studies, Planetary science, Exploration of Jupiter, Gravitational field, Space and Planetary Science, law, symbols, Satellite, Aerospace engineering, business, Titan (rocket family), Saturnian system
Abstract

The Cassini mission to Saturn employs a Saturn orbiter and a Titan probe to conduct an intensive investigation of the Saturnian system. The orbiter flies a series of orbits, incorporating flybys of the Saturnian satellites, called the ‘satellite tour.’ During the tour, the gravitational fields of the satellites (mainly Titan) are used to modify and control the orbit, targeting from one satellite flyby to the next. The tour trajectory must also be designed to maximize opportunities for a diverse set of science observations, subject to mission-imposed constraints. Tour design studies have been conducted for Cassini over a period of several years to identify trades and strategies for achieving these sometimes conflicting goals. Concepts, strategies, and techniques previously developed for the Galileo mission to Jupiter have been modified, and new ones have been developed, to meet the requirements of the Cassini mission. A sample tour is presented illustrating the application of tour design strategies developed for Cassini.

Published
2002
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50. The exploration of Titan with an orbiter and a lake probe

Author

Rosaly M. C. Lopes, Gilbert Fanchini, Roberto Orosei, Luciano Iess, Tetsuya Tokano, Gabriel Tobie, Jean-Pierre Lebreton, Maria Luisa Moriconi, Ralph D. Lorenz, Ellen R. Stofan, R. Meriggiola, Giuseppe Mitri, Federico Tosi, Krishan K. Khurana, Christophe Sotin, Athena Coustenis, Alexander Hayes, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Smart Structures Solutions S.r.l., Rome, Italy, Université Paris Diderot - Paris 7 (UPD7), Department of Astronomy [Ithaca], Cornell University [New York], Dipartimento di Ingegneria Meccanica e Aerospaziale [Roma La Sapienza] (DIMA), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Istituto di Scienze dell'Atmosfera e del Clima (ISAC), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Freie Universität Berlin, Centre de Formation et de Recherche sur les Environnements Méditérranéens (CEFREM), Université de Perpignan Via Domitia (UPVD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Proxemy Research Inc, Institut für Geophysik und Meteorologie [Köln], Universität zu Köln = University of Cologne, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], University of California-University of California, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Consiglio Nazionale delle Ricerche [Roma] (CNR), Université de Perpignan Via Domitia (UPVD)-Centre National de la Recherche Scientifique (CNRS), and Universität zu Köln

Subjects
010504 meteorology & atmospheric sciences, 7. Clean energy, 01 natural sciences, law.invention, Astrobiology, Physics::Geophysics, Orbiter, symbols.namesake, law, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Saturnian system, Habitability, Astronomy and Astrophysics, Titan, Space and Planetary Science, Prebiotic chemistry, 13. Climate action, [SDU]Sciences of the Universe [physics], Physics::Space Physics, symbols, Environmental science, Astrophysics::Earth and Planetary Astrophysics, Titan (rocket family), Rotational dynamics
Abstract

International audience; Fundamental questions involving the origin, evolution, and history of both Titan and the broader Saturnian system can be answered by exploring this satellite from an orbiter and also in situ. We present the science case for an exploration of Titan and one of its lakes from a dedicated orbiter and a lake probe. Observations from an orbit-platform can improve our understanding of Titan׳s geological processes, surface composition and atmospheric properties. Further, combined measurements of the gravity field, rotational dynamics and electromagnetic field can expand our understanding of the interior and evolution of Titan. An in situ exploration of Titan׳s lakes provides an unprecedented opportunity to understand the hydrocarbon cycle, investigate a natural laboratory for prebiotic chemistry and habitability potential, and study meteorological and marine processes in an exotic environment. We briefly discuss possible mission scenarios for a future exploration of Titan with an orbiter and a lake probe. •We present the science case for Titan׳s exploration.•We present mission scenarios for a future exploration of Titan.•This paper is based on a white paper presented for 2013 ESA׳s Call for Large missions.

Published
2014
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