Other
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008epsc.conf..797m&link_type=abstract
European Planetary Science Congress 2008, Proceedings of the conference held 21-25 September, 2008 in Münster, Germany. Online a
Other
Scientific paper
ABSTRACT The current orbits of the Earth and Venus are nearly circular and coplanar whereas orbits of asteroids are highly eccentric and inclined. The most of the mass of the inner solar system (inside the Jupiter's orbit) is contained in the Earth and Venus with the spatially narrow separation and the total mass of asteroids is only of the order of 10-4 earth mass, suggesting strong depletion during their formation. Although some of previousmodels, primarily based on N-body simulations, suceeded to reproduce a part of such characteristics, there is no model, which can satisfy all of characteristics. In the present study, we have conducted series of N- body simulations with wide range of physical parameters, using a fast N-body code we have recently developed. In simulations, 2000 equal-mass planetesimals are initially placed between 0.5-4.0AU, and collisional growth is followed until the end of accretion (> 100Myr), with the full self-gravity and the effects of gas: the gas drag, tidal interaction (including Type I migration), and nebular potential. The physical parameters for simulations are as follows: (1) the time scale of gas dissipation ( = 1,2,3,and 5 Myr), (2) the initial spatial distribution of solid material (the total mass of 5 and 10 earth mass and the power-law index for the radial profile of the surface density, p = -1 and -2), and (3) initial orbits of Jupiter and Saturn (present orbits giant planets, PJS1, those from the Nice model, NJS1, and the cases of the same semimajor axes with PJS1 and NJS1, respectively, but with larger orbital eccentricities, PJS2 and NJS2). We find that outcome of simulations strongly depends on and orbits of giant planets and weakly on the initial spatial distribution of planetesimals. In order to hold a total mass similar to that for the current inner solar system ( 2 earth mass), needs to be 1-3Myr. For the case of NJS simulations in which the orbital separation of Jupiter and Saturn is as small as that suggested from the Nice model, since the secular resonance with Jupiter migrates from 3AU to only 2AU, we inevitably have a large planet slightly inside of 2AU. It seems difficult to remove this planet in any later events. On the other hand, for the case of PJS simulations, final planets are spatially more confined around 1AU than the case of NJS simulations, since the secular resonance can reach to 0.7AU [1, 2]. However, the secular resonance completely sweeps up all bodies initially located between 2AU and 3AU (they all migrate inward) in PJS simulations. This looks inconsistent with the current orbital distribution of asteroids, while NJS simulations (in particular NJS1 simulations) seem to give more consistent orbital distributions. The accretion time scale is shorter in PJS simulations than NJS simulations as suggested from previous studies [3]. In the presentation, we will discuss possible scenarios which can reproduce both orbits of terrestrial planets and asteroids consistently with their present states. References [1] Nagasawa, M. Lin, D.N.C. and Thommes E. (2005), ApJ, 635, 578-598. [2] Thommes E, Nagasawa, M. and Lin, D.N.C. (2008), ApJ, 676, 728-739. [3] O'brien, D.P. Morbidelli, A. and Levison, H.F. (2006), Icarus, 184, 39-58
Moore Ben
Morishima Ryuji
Schmidt Max W.
Stadel Joachim
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