EMERGENCE OF PROTOPLANETARY DISKS AND SUCCESSIVE FORMATION OF GASEOUS PLANETS BY GRAVITATIONAL INSTABILITY

2009/12/31 by Shu-ichiro Inutsuka, Shu‐ichiro Inutsuka, Masahiro N. Machida +1 · 5 citations
Physics and Astronomy · #Accretion (finance) #Astro and Planetary Science #Astrobiology #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Galaxy #Giant planet #Gravitational instability #Instability #Mechanics #Molecular cloud #Physics #Planet #Planetary migration #Planetary system #Planetesimal #Protoplanetary disk #Protostar #Star formation #Stars #Stellar, planetary, and galactic studies #Terrestrial planet #astro-ph.EP #astro-ph.SR

paper · pdf · doi:10.1088/2041-8205/718/2/l58

12 pages, 3 figures, ApJL in press

arxiv created 2010/06/29 · openalex publication_date 2010/07/06 · arxiv updated 2015/05/14 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05

Abstract

We use resistive magnetohydrodynamical (MHD) simulations with the nested grid technique to study the formation of protoplanetary disks around protostars from molecular cloud cores that provide the realistic environments for planet formation. We find that gaseous planetary-mass objects are formed in the early evolutionary phase by gravitational instability in regions that are decoupled from the magnetic field and surrounded by the injection points of the MHD outflows during the formation phase of protoplanetary disks. Magnetic decoupling enables massive disks to form and these are subject to gravitational instability, even at ∼10 AU. The frequent formation of planetary-mass objects in the disk suggests the possibility of constructing a hybrid planet formation scenario, where the rocky planets form later under the influence of the giant planets in the protoplanetary disk.

Citations

• DISCOVERY OF THE COLDEST IMAGED COMPANION OF A SUN-LIKE STAR
• Optical Images of an Exosolar Planet 25 Light-Years from Earth
• Mechanism of Magnetic Flux Loss in Molecular Clouds
• The conductivity of dense molecular gas
• Direct Imaging of Multiple Planets Orbiting the Star HR 8799
• Models of Jupiter's Growth Incorporating Thermal and Hydrodynamic Constraints
• Numerical Calculations of the Dynamics of a Collapsing Proto-Star*

Cited by

• FORMATION PROCESS OF THE CIRCUMSTELLAR DISK: LONG-TERM SIMULATIONS IN THE MAIN ACCRETION PHASE OF STAR FORMATION
• Infrared Search for Young Brown Dwarf Companions around Young Stellar Objects in the ρ Ophiuchi and the Serpens Molecular Clouds
• Episodic accretion: the interplay of infall and disc instabilities
• Formation of terrestrial planet cores inside giant planet embryos
• Recent Developments in Simulations of Low-mass Star Formation

Related

• Simulations of unstable gaseous disks and the origin of giant planets
• Dynamics of Protoplanetary Disks
• Zooming in on the Formation of Protoplanetary Disks
• Giant planet formation from disk instability; cooling and heating
• A semi-analytical model of the outer structure of protoplanetary discs formed by the collapse of a rotating molecular cloud