Giant planet formation from disk instability cooling and heating

被引：0

作者：

Mayer, L ^{[1
]}

Wadsley, J ^{[1
]}

Quinn, T ^{[1
]}

Stadel, J ^{[1
]}

机构：

[1] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland

来源：

Extrasolar Planets: Today and Tomorrow | 2004年 / 321卷

关键词：

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the results of high resolution SPH simulations of the evolution of gravitationally unstable protoplanetaxy disks. We report on calculations in which the disk is evolved using a locally isothermal or adiabatic equation of state (with shock heating), and also on new simulations in which cooling and heating by radiation are explicitly modeled. We find that disks with a minimum Toomre parameter < 1.4 fragment into several gravitationally bound protoplanets with masses from below to a few Jupiter masses. This is confirmed also in runs where the disk is given a quiet start, growing gradually in mass over several orbital times. A cooling time comparable to the orbital time is needed to achieve fragmentation, for disk masses in the range 0.08 - 0.1 M-circle dot. After about 30 orbital times, merging between the bound condensations always leads to 2-3 protoplanets on quite eccentric orbits.

引用

页码：290 / 297

页数：8

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