Astronomy and Astrophysics – Astrophysics – Solar and Stellar Astrophysics
Scientific paper
2009-06-08
Astrophys.J.701:620-634,2009
Astronomy and Astrophysics
Astrophysics
Solar and Stellar Astrophysics
Accepted by ApJ. Simulation movies can be downloaded at: http://www.astro.lsa.umich.edu/~zhuzh/research.html
Scientific paper
10.1088/0004-637X/701/1/620
We have developed time-dependent models of FU Ori accretion outbursts to explore the physical properties of protostellar disks. Our two-dimensional, axisymmetric models incorporate full vertical structure with a new treatment of the radiative boundary condition for the disk photosphere. We find that FU Ori-type outbursts can be explained by a slow accumulation of matter due to gravitational instability. Eventually this triggers the magnetorotational instability, which leads to rapid accretion. The thermal instability is triggered in the inner disk but this instability is not necessary for the outburst. An accurate disk vertical structure, including convection, is important for understanding the outburst behavior. Large convective eddies develop during the high state in the inner disk. The models are in agreement with Spitzer IRS spectra and also with peak accretion rates and decay timescales of observed outbursts, though some objects show faster rise timescale. We also propose that convection may account for the observed mild-supersonic turbulence and the short-timescale variations of FU Orionis objects.
Gammie Charles
Hartmann Lee
McKinney Jonathan C.
Zhu Zhaohuan
No associations
LandOfFree
2-D simulations of FU Orionis disk outbursts 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 2-D simulations of FU Orionis disk outbursts, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and 2-D simulations of FU Orionis disk outbursts will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-64256