Other
Scientific paper
Aug 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1158...23m&link_type=abstract
EXOPLANETS AND DISKS: THEIR FORMATION AND DIVERSITY: Proceedings of the International Conference. AIP Conference Proceedings, V
Other
Interstellar Dust Grains, Diffuse Emission, Infrared Cirrus, Magnetic And Electric Fields, Polarization Of Starlight, Atmospheres, Hydrodynamics
Scientific paper
Protoplanetary disk formation is investigated by three-dimensional hydrodynamic simulations. We directly calculate the disk formation from the molecular cloud core, in which about five orders of magnitude of spatial scale is resolved using a nested grid method. We parameterized the rotational energy of the cloud core, and calculated the disk about ~105 yr after the protostar formation. After the protoplanetary disk becomes unstable against gravity, fragmentation occurs to form gas giant planets when the cloud core has a larger rotational energy at the initial state. On the other hand, a stable disk maintains for ~105 yr after the protostar formation when the cloud core has a smaller rotational energy. Comparison of observations with our results indicate that gas planets are frequently formed through the gravitational instability in the protoplanetary disk, which possibly accounts for the formation of gas giant planets located far from the central star.
Inutsuka Shu-ichiro
Machida Masahiro N.
Matsumoto Tomoaki
No associations
LandOfFree
Protoplanetary Disk Formation in Molecular Cloud Cores does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Protoplanetary Disk Formation in Molecular Cloud Cores, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Protoplanetary Disk Formation in Molecular Cloud Cores will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1313555