2013/06/28 by Patryk Sofia Lykawka, Takashi Ito, Takashi Itô · 53 citations
Physics and Astronomy · #Astro and Planetary Science #Astrobiology #Astronomy #Astrophysics #Geology #Giant planet #Jupiter (rocket family) #Jupiter mass #Mars Exploration Program #Nice model #Physics #Planet #Planetary Science and Exploration #Planetary mass #Planetary migration #Planetary system #Planetesimal #Saturn #Stellar, planetary, and galactic studies #Terrestrial planet #astro-ph.EP
paper · pdf · doi:10.1088/0004-637x/773/1/65
published in The Astrophysical Journal 773(1), 65 (IOP Publishing) · 32 pages, 11 figures, 1 table. Accepted for publication in ApJ (Proof corrected version)
arxiv created 2013/06/28 · openalex publication_date 2013/07/26 · arxiv updated 2013/08/05 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
The newly formed giant planets may have migrated and crossed a number of mutual mean motion resonances (MMRs) when smaller objects (embryos) were accreting to form the terrestrial planets in the planetesimal disk.We investigated the effects of the planetesimal-driven migration of Jupiter and Saturn, and the influence of their mutual 1:2 MMR crossing on terrestrial planet formation for the first time, by performing N-body simulations.These simulations considered distinct timescales of MMR crossing and planet migration.In total, 68 high-resolution simulation runs using 2000 disk planetesimals were performed, which was a significant improvement on previously published results.Even when the effects of the 1:2 MMR crossing and planet migration were included in the system, Venus and Earth analogs (considering both orbits and masses) successfully formed in several runs.In addition, we found that the orbits of planetesimals beyond a ∼ 1.5-2 AU were dynamically depleted by the strengthened sweeping secular resonances associated with Jupiter's and Saturn's more eccentric orbits (relative to the present day) during planet migration.However, this depletion did not prevent the formation of massive Mars analogs (planets with more than 1.5 times Mars's mass).Although late MMR crossings (at t > 30 Myr) could remove such planets, Mars-like small mass planets survived on overly excited orbits (high e and/or i), or were completely lost in these systems.We conclude that the orbital migration and crossing of the mutual 1:2 MMR of Jupiter and Saturn are unlikely to provide suitable orbital conditions for the formation of solar system terrestrial planets.This suggests that to explain Mars's small mass and the absence of other planets between Mars and Jupiter, the outer asteroid belt must have suffered a severe depletion due to interactions with Jupiter/Saturn, or by an alternative mechanism (e.g., rogue super-Earths).