Clumps in the outer disk by disk instability: Why they are initially gas giants and the legacy of disruption

被引：179

作者：

Boley, Aaron C. ^{[1
,2
]}

Hayfield, Tristen ^{[3
]}

Mayer, Lucio ^{[2
]}

Durisen, Richard H. ^{[4
]}

机构：

[1] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA

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

[3] ETH, Dept Phys, CH-8093 Zurich, Switzerland

[4] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA

来源：

ICARUS | 2010年 / 207卷 / 02期

关键词：

Disks; Planetary formation; Planets; Migration; Planetesimals; SMOOTHED PARTICLE HYDRODYNAMICS; PROTOPLANETARY DISKS; FU-ORIONIS; GRAVITATIONAL INSTABILITIES; PLANET FORMATION; BROWN DWARFS; SOLAR NEBULA; FRAGMENTATION; ACCRETION; STARS;

D O I：

10.1016/j.icarus.2010.01.015

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We explore the initial conditions for fragments in the extended regions (r greater than or similar to 50 AU) of gravitationally unstable disks. We combine analytic estimates for the fragmentation of spiral arms with 3D SPH simulations to show that initial fragment masses are in the gas giant regime. These initial fragments will have substantial angular momentum, and should form disks with radii of a few AU. We show that clumps will survive for multiple orbits before they undergo a second, rapid collapse due to H(2) dissociation and that it is possible to destroy bound clumps by transporting them into the inner disk. The consequences of disrupted clumps for planet formation, dust processing, and disk evolution are discussed. We argue that it is possible to produce Earth-mass cores in the outer disk during the earliest phases of disk evolution. (C) 2010 Elsevier Inc. All rights reserved.

引用

页码：509 / 516

页数：8