Dust circulation by radiation pressure in protoplanetary disks with puffed up inner rim
| Autor: | Fujiwara, Daisuke, Watanabe, Seiichiro |
|---|---|
| Jazyk: | angličtina |
| Rok vydání: | 2006 |
| Předmět: |
density distribution
protoplanetary disk gravitational instability 計算機シミュレーション Astrophysics::Cosmology and Extragalactic Astrophysics radiation pressure 密度分布 放射圧 Astrophysics::Solar and Stellar Astrophysics 宇宙塵 Astrophysics::Galaxy Astrophysics 循環 惑星間塵 cosmic dust turbulence 重力不安定性 protoplanet stellar luminosity 原始惑星系円盤 原始惑星 乱流 恒星光度 circulation Astrophysics::Earth and Planetary Astrophysics interplanetary dust computerized simulation |
| Zdroj: | 第38回月・惑星シンポジウム = Proceedings of the 38th ISAS Lunar and Planetary Symposium. :124-127 |
| Popis: | We perform numerical simulations of the radial circulation of the dust in weak turbulent protoplanetary disks, taking the effect of radiation pressure of the central star and puffed-up inner rim of the disk into account. We confirm that the following dust circulation mechanism will be realized: at the inner edge of the disk, the infalling dust aggregates partially evaporate and break up into fine grains, which are stirred up to the upper irradiated region by magnetorotational instability and are blown outward by the radiation pressure. Most of the blowing grains reenter into the disk within approximately 1 AU and settle to the midplane, joining inwardly-migrating dust aggregates. We find that in the shadowed region of the disk the outflow mass flux in the surface layer is comparable to the inflow mass flux in the disk interior. Dust circulation occurs efficient in the shadowed region if the turbulent intensity in the innermost region of the disk and the stellar luminosity are sufficient higher. In a steady state, the surface density distribution of the dust is enhanced by dust circulation in the inner shadowed region. Therefore, the enhanced abundance of the dust may cause gravitational instability for planetesimal formation. 資料番号: AA0063350034 |
| Databáze: | OpenAIRE |
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