| Co-Investigator(Kenkyū-buntansha) |
二村 徳宏 特定非営利活動法人日本スペースガード協会(スペースガード研究センター), スペースガード部門, 研究員 (60771483)
佐々木 貴教 京都大学, 理学研究科, 助教 (70614064)
片岡 龍峰 国立極地研究所, 研究教育系, 准教授 (90462671)
飯高 敏晃 国立研究開発法人理化学研究所, 情報システム本部, 専任研究員 (60212700)
塩田 大幸 名古屋大学, 太陽地球環境研究所, 研究員 (90462192)
|
|---|
| Budget Amount *help |
¥117,650,000 (Direct Cost: ¥90,500,000、Indirect Cost: ¥27,150,000)
Fiscal Year 2018: ¥23,530,000 (Direct Cost: ¥18,100,000、Indirect Cost: ¥5,430,000)
Fiscal Year 2017: ¥23,530,000 (Direct Cost: ¥18,100,000、Indirect Cost: ¥5,430,000)
Fiscal Year 2016: ¥23,530,000 (Direct Cost: ¥18,100,000、Indirect Cost: ¥5,430,000)
Fiscal Year 2015: ¥23,530,000 (Direct Cost: ¥18,100,000、Indirect Cost: ¥5,430,000)
Fiscal Year 2014: ¥23,530,000 (Direct Cost: ¥18,100,000、Indirect Cost: ¥5,430,000)
|
|---|
| Outline of Final Research Achievements |
We constructed one-dimensional model which describes the evolution of proto-planetary disk. We determined the steady-state solution of accretion disk, based on the formulation by Shakura and Sunyaev (1973) and found that the structure of the protoplanetary disk is determined mainly by Magneto-rotational instability (MRI) and divided into three regions, those are outer turbulent region, MRI inactive region, and inner turbulent region. At the two boundaries of the MRI inactive region (outer and inner boundaries), planets are formed from solid particles and rapidly grow by “pebbles” accretion onto them. Icy planets and gas giant cores form at the outer boundary and rocky planets at the inner boundary. We named this theory as “Tandem planet formation theory” to distinguish the previous theories.
|
