2006/12/21 by Masahiro Ogihara, Shigeru Ida, Alessandro Morbidelli · 3 citations
Physics and Astronomy · #Accretion (finance) #Astro and Planetary Science #Astrobiology #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Exoplanet #Formation and evolution of the Solar System #Physics #Planet #Planetary mass #Planetary migration #Protoplanet #Protoplanetary disk #Solar System #Stellar, planetary, and galactic studies #Terrestrial planet #Venus #astro-ph
paper · pdf · doi:10.1016/j.icarus.2006.12.006
accepted for publication in Icarus; 19 pages, 8 figures, 1 table
arxiv created 2006/12/21 · openalex publication_date 2007/01/05 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We have investigated the final accretion stage of terrestrial planets from Mars-mass protoplanets that formed through oligarchic growth in a disk comparable to the minimum mass solar nebula (MMSN), through N-body simulation including random torques exerted by disk turbulence due to Magneto-Rotational-Instability. For the torques, we used the semi-analytical formula developed by Laughlin et al.(2004). The damping of orbital eccentricities (in all runs) and type-I migration (in some runs) due to the tidal interactions with disk gas are also included. We found that the orbital eccentricities pumped up by the turbulent torques and associated random walks in semimajor axes tend to delay isolation of planets, resulting in more coagulation of planets than in the case without turbulence. The eccentricities are still damped after planets become isolated. As a result, the number of final planets decreases with increase in strength of the turbulence, while Earth-mass planets with small eccentricities are still formed. In the case of relatively strong turbulence, the number of final planets are 4-5 at 0.5-2AU, which is consistent with Solar system, for relatively wide range of disk surface density (~10-4-10-2 times MMSN).