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A scenario of Jupiter system formation. First phase: Jupiter forms, its Hill and outer radii coincide, and no subnebula can exist (first line). Second phase: formation of the satellite system. A subnebula appears, fed in its infancy by gas and gas-coupled solids originating from the solar. Planetesimals, some of them having lost their volatile due to temperature and pressure conditions prevailing in the subnebula, grow to form satellites (second and third lines). When the subnebula disappears (fourth line), the irregular satellites are captured
The first phase (first line in Fig. 2 ), the
formation of Jupiter, took place during the nebular epoch of Solar
System history, when the gaseous component was still present and
the solid component was slowly giving birth to planetesimals by
means of accumulation processes.
The second phase (second to fourth lines in Fig. 2 )
begins when Jupiter’s region of gravitational influence (quantified
by its Hill’s radius) enlarges and exceeds its outer radius.
The captured planetesimals then can grow further in mass due to
mutual collisions and build up the regular Jovian satellites
(Fig. 2 , second and third lines): the content of ices can
vary from satellite to satellite, since part of the original
planetesimals could have lost their volatile species (in particular
water ice) due to the temperature and pressure condition prevailing
in the Jovian subnebula [ 63 ].
Blanc, Michel; Alibert, Yann; André, Nicolas; Atreya, Sushil; Beebe, Reta; Benz, Willy; Bolton, Scott J.; Coradini, Angioletta; Coustenis, Athena; Dehant, Véronique; Dougherty, Michele; Drossart, Pierre; Fujimoto, Masaki; Grasset, Olivier; Gurvits, Leonid; Hartogh, Paul; Hussmann, Hauke; Kasaba, Yasumasa; Kivelson, Margaret; Khurana, Krishan; Krupp, Norbert; Louarn, Philippe; Lunine, Jonathan; McGrath, Melissa; Mimoun, David; Mousis, Olivier; Oberst, Juergen; Okada, Tatsuaki; Pappalardo, Robert; Prieto-Ballesteros, Olga; Prieur, Daniel; Regnier, Pascal; Roos-Serote, Maarten; Sasaki, Sho; Schubert, Gerald; Sotin, Christophe; Spilker, Tom; Takahashi, Yukihiro; Takashima, Takeshi; Tosi, Federico; Turrini, Diego; Hoolst, Tim; Zelenyi, LevJournal: Experimental Astronomy
Issue 3DOI: 10.1007/s10686-008-9127-4Published: 2009-02-18Institution(s):
CESR (UPS/CNRS), Ecole Polytechnique, University of Bern, Institut UTINAM, European Space Agency, University of Michigan, New Mexico State University, SwRI, INAF—Istituto di Fisica dello Spazio Interplanetario, LESIA, Royal Observatory of Belgium, Imperial College, Japan Aerospace Exploration Agency (JAXA), Université de Nantes, JIVE, DLR Institute of Planetary Research, Tohoku University, University of California, Max-Planck-Institut für Sonnensystemforschung, University of Arizona, NASA/Marshall Spaceflight Center, Université de Toulouse, ISAE-SUPAERO, DLR, NASA/JPL, Centro de Astrobiologia-INTA-CSIC, Université de Bretagne Occidentale, EADS/ASTRIUM, National Astronomical Observatory, Jet Propulsion Laboratory, Space Research Institute (IKI)
The exploration of the Jovian System and its fascinating satellite Europa is one of the priorities presented in ESA’s “Cosmic Vision” strategic document. The Jovian System indeed displays many facets. It is a small planetary system in its own right, built-up out of the mixture of gas and icy material that was present in the external region of the solar nebula. Through a complex history of accretion, internal differentiation and dynamic interaction, a very unique satellite system formed, in which three of the four Galilean satellites are locked in the so-called Laplace resonance. The energy and angular momentum they exchange among themselves and with Jupiter contribute to various degrees to the internal heating sources of the satellites. Unique among these satellites, Europa is believed to shelter an ocean between its geodynamically active icy crust and its silicate mantle, one where the main conditions for habitability may be fulfilled. For this very reason, Europa is one of the best candidates for the search for life in our Solar System. So, is Europa really habitable, representing a “habitable zone” in the Jupiter system? To answer this specific question, we need a dedicated mission to Europa. But to understand in a more generic way the habitability conditions around giant planets, we need to go beyond Europa itself and address two more general questions at the scale of the Jupiter system: to what extent is its possible habitability related to the initial conditions and formation scenario of the Jovian satellites? To what extent is it due to the way the Jupiter system works? ESA’s Cosmic Vision programme offers an ideal and timely framework to address these three key questions. Building on the in-depth reconnaissance of the Jupiter System by Galileo (and the Voyager, Ulysses, Cassini and New Horizons fly-by’s) and on the anticipated accomplishments of NASA’s JUNO mission, it is now time to design and fly a new mission which will focus on these three major questions. LAPLACE, as we propose to call it, will deploy in the Jovian system a triad of orbiting platforms to perform coordinated observations of its main components: Europa, our priority target, the Jovian satellites, Jupiter’s magnetosphere and its atmosphere and interior. LAPLACE will consolidate Europe’s role and visibility in the exploration of the Solar System and will foster the development of technologies for the exploration of deep space in Europe. Its multi-platform and multi-target architecture, combined with its broadly multidisciplinary scientific dimension, will provide an outstanding opportunity to build a broad international collaboration with all interested nations and space agencies.
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