CONSTRAINT ON THE GIANT PLANET PRODUCTION BY CORE ACCRETION

被引:64
作者
Rafikov, Roman R. [1 ]
机构
[1] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08540 USA
关键词
planetary systems; planets and satellites: formation; protoplanetary disks; PROTOPLANETARY ATMOSPHERES; SOLAR NEBULA; WIDE ORBITS; GAS; DISKS; MASS; INSTABILITY; EVOLUTION; OPACITY; FRAGMENTATION;
D O I
10.1088/0004-637X/727/2/86
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The issue of giant planet formation by core accretion (CA) far from the central star is rather controversial because the growth of a massive solid core necessary for triggering the gas runaway can take longer than the lifetime of the protoplanetary disk. In this work, we assess the range of separations at which CA may operate by (1) allowing for an arbitrary (physically meaningful) rate of planetesimal accretion by the core and (2) properly taking into account the dependence of the critical mass for the gas runaway on the planetesimal accretion luminosity. This self-consistent approach distinguishes our work from similar studies in which only a specific planetesimal accretion regime was explored and/or the critical core mass was fixed at some arbitrary level. We demonstrate that the largest separation at which the gas runaway can occur within 3 Myr corresponds to the surface density of solids in the disk greater than or similar to 0.1 g cm(-2) and is 40-50 AU in the minimum mass solar nebula. This limiting separation is achieved when the planetesimal accretion proceeds at the fastest possible rate, even though the high associated accretion luminosity increases the critical core mass, delaying the onset of gas runaway. Our constraints are independent of the mass of the central star and vary only weakly with the core density and its atmospheric opacity. We also discuss various factors that can strengthen or weaken our limits on the operation of CA.
引用
收藏
页数:8
相关论文
共 40 条
[1]   Models of giant planet formation with migration and disc evolution [J].
Alibert, Y ;
Mordasini, C ;
Benz, W ;
Winisdoerffer, C .
ASTRONOMY & ASTROPHYSICS, 2005, 434 (01) :343-353
[2]   THE TWO MODES OF GAS GIANT PLANET FORMATION [J].
Boley, Aaron C. .
ASTROPHYSICAL JOURNAL LETTERS, 2009, 695 (01) :L53-L57
[3]   On the formation of gas giant planets on wide orbits [J].
Boss, AP .
ASTROPHYSICAL JOURNAL, 2006, 637 (02) :L137-L140
[4]   Evolution of the solar nebula. IV. Giant gaseous protoplanet formation [J].
Boss, AP .
ASTROPHYSICAL JOURNAL, 1998, 503 (02) :923-937
[5]   PHYSICS OF PRIMITIVE SOLAR ACCRETION DISK [J].
CAMERON, AGW .
MOON AND THE PLANETS, 1978, 18 (01) :5-40
[6]   Spectral energy distributions of T Tauri stars with passive circumstellar disks [J].
Chiang, EI ;
Goldreich, P .
ASTROPHYSICAL JOURNAL, 1997, 490 (01) :368-376
[7]   Pseudo-viscous modelling of self-gravitating discs and the formation of low mass ratio binaries [J].
Clarke, C. J. .
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2009, 396 (02) :1066-1074
[8]   THE FORMATION MECHANISM OF GAS GIANTS ON WIDE ORBITS [J].
Dodson-Robinson, Sarah E. ;
Veras, Dimitri ;
Ford, Eric B. ;
Beichman, C. A. .
ASTROPHYSICAL JOURNAL, 2009, 707 (01) :79-88
[9]   ON THE ORIGIN OF PLANETARY SPINS [J].
DONES, L ;
TREMAINE, S .
ICARUS, 1993, 103 (01) :67-92
[10]   Nonlinear outcome of gravitational instability in cooling, gaseous disks [J].
Gammie, CF .
ASTROPHYSICAL JOURNAL, 2001, 553 (01) :174-183