Other
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21742902p&link_type=abstract
American Astronomical Society, AAS Meeting #217, #429.02; Bulletin of the American Astronomical Society, Vol. 43, 2011
Other
Scientific paper
There has been disagreement about whether cooling in protoplanetary disks can be sufficiently fast to induce the formation of gas giant protoplanets via gravitational instabilities. Simulations by our own group and others indicate that this method of planet formation does not work for disks around young, low-mass stars inside several tens of AU, while simulations by other groups show fragmentation into protoplanetary clumps in this region. To allow direct comparison in hopes of isolating the cause of the differences, we here present a comparison high-resolution three-dimensional hydrodynamics simulation of a protoplanetary disk,using an improved version of one of our own radiative schemes. We find that the disk does not fragment in our code but instead quickly settles into a state with only low amplitude nonaxisymmetric structure, which persists for at least several outer disk rotations. Further, we see no rapid radiative or convective cooling.
Cai Kai
Durisen Richard
Milne Margaret
Pickett Megan K.
No associations
LandOfFree
Comparison Simulations of Gas Giant Planet Formation via Disk Instability 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 Comparison Simulations of Gas Giant Planet Formation via Disk Instability, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Comparison Simulations of Gas Giant Planet Formation via Disk Instability will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1404008