The effects of metallicity and grain growth and settling on the early evolution of gaseous protoplanets
暂无分享,去创建一个
[1] J. Pollack,et al. A calculation of the Rosseland mean opacity of dust grains in primordial solar system nebulae , 1985 .
[2] P. Bodenheimer,et al. Formation of Jupiter using opacities based on detailed grain physics , 2010, 1005.3875.
[3] C. Tropea,et al. Light Scattering from Small Particles , 2003 .
[4] J. M. Irvine. Protostars and Planets – Studies of Star Formation and of the Origin of the Solar System , 1979 .
[5] K. Rice,et al. Protostars and Planets V , 2005 .
[6] Roman R. Rafikov. Convective cooling and fragmentation of gravitationally unstable disks , 2007 .
[7] A. Boss. Evolution of the Solar Nebula. V. Disk Instabilities with Varied Thermodynamics , 2002 .
[8] Jack J. Lissauer,et al. Formation of the Giant Planets by Concurrent Accretion of Solids and Gas , 1995 .
[9] B. Macintosh,et al. Direct Imaging of Multiple Planets Orbiting the Star HR 8799 , 2008, Science.
[10] Mark Clampin,et al. Optical Images of an Exosolar Planet 25 Light-Years from Earth , 2008, Science.
[11] A. Cameron. Physics of the primitive solar nebula and of giant gaseous protoplanets , 1978 .
[12] Aaron C. Boley,et al. ON THE POSSIBILITY OF ENRICHMENT AND DIFFERENTIATION IN GAS GIANTS DURING BIRTH BY DISK INSTABILITY , 2010, Proceedings of the International Astronomical Union.
[13] Jack J. Lissauer,et al. Accretion of the gaseous envelope of Jupiter around a 5–10 Earth-mass core , 2005 .
[14] J. Pollack,et al. Interactions of planetesimals with protoplanetary atmospheres , 1988 .
[15] M. Podolak. The contribution of small grains to the opacity of protoplanetary atmospheres , 2003 .
[16] Charles F. Gammie,et al. Nonlinear Outcome of Gravitational Instability in Cooling, Gaseous Disks , 2001, astro-ph/0101501.
[17] Ravit Helled,et al. Grain sedimentation in a giant gaseous protoplanet , 2008, 0801.2435.
[18] A. Cameron,et al. Structure and evolution of isolated giant gaseous protoplanets , 1979 .
[19] N. Movshovitz,et al. The opacity of grains in protoplanetary atmospheres , 2007, 0710.0096.
[20] James Wadsley,et al. Fragmentation of Gravitationally Unstable Gaseous Protoplanetary Disks with Radiative Transfer , 2007 .
[21] Aaron C. Boley,et al. Clumps in the outer disk by disk instability: Why they are initially gas giants and the legacy of disruption , 2009, 0909.4543.
[22] R. Durisen,et al. GIANT PLANET FORMATION BY DISK INSTABILITY: A COMPARISON SIMULATION WITH AN IMPROVED RADIATIVE SCHEME , 2009, 0907.4213.
[23] R. Rafikov,et al. PROPERTIES OF GRAVITOTURBULENT ACCRETION DISKS , 2009, 0901.4739.
[24] J. Cuzzi,et al. Closed-form expressions for particle relative velocities induced by turbulence , 2007, astro-ph/0702303.
[25] S. Michael,et al. The Effects of Metallicity and Grain Size on Gravitational Instabilities in Protoplanetary Disks , 2005, astro-ph/0508354.
[26] A. Boss. Flux-limited Diffusion Approximation Models of Giant Planet Formation by Disk Instability , 2008, 0801.4371.
[27] F. Meru,et al. Exploring the conditions required to form giant planets via gravitational instability in massive protoplanetary discs , 2010, 1004.3766.
[28] P. Bodenheimer,et al. Calculations of the evolution of the giant planets , 1980 .
[29] Eric B. Ford,et al. THE FORMATION MECHANISM OF GAS GIANTS ON WIDE ORBITS , 2009, 0909.2662.
[30] P. Bodenheimer,et al. Metallicity of the massive protoplanets around HR 8799 If formed by gravitational instability , 2009, 0911.5003.
[31] Alan P. Boss,et al. Giant Planet Formation by Gravitational Instability , 1997 .
[32] Aaron C. Boley,et al. THE TWO MODES OF GAS GIANT PLANET FORMATION , 2009, 0902.3999.
[33] David R. Alexander,et al. Low-Temperature Rosseland Opacities , 1975 .
[34] Ravit Helled,et al. Planetesimal capture in the disk instability model , 2006 .