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: http://ip.rsu.ru/~vorobyov/project3.htm
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The susceptibility of protostellar disks to gravitational instability and
subsequent formation of protoplanetary clumps is currently under debate. We
perform numerical simulations of the gravitational cloud core collapse until
approximately 99% of the initial cloud core mass is accreted by the central
protostar and protostellar disk system. We find that the protostellar disk is
gravitationally unstable, even in the later phase of negligible mass infall from
the surrounding envelope, and quickly develops a flocculent spiral structure.
The spiral structure is sharp in the early phase of disk evolution and is
diffuse in the later phase. In the early phase when the mass infall from the
envelope is sufficiently high, dense protoplanetary clumps form within the spiral
arms. Some of the clumps get dispersed during several orbital periods and the
others are driven onto the protostar. These episodes of clump infall can
increase the luminosity of the protostar by several orders
of magnitude.
The results are accepted for publication in Astrophysical Journal Letters.
This research was done in collaboration with
Prof. Shantanu Basu.
UPPER PANEL: The gas surface density map in log scale.
The red circle in the center represents the central protostar. The development of spiral
structure in the protostellar disk is evident. Dense protostellar/protoplanetary
clumsp form within the spiral arms and are driven into the protostar by the action
of gravitational torques.
LOWER PANEL: The mass accretion rate onto the protostar as a function of time. The mass accretion rate is characterized by very short (<100 yr) but vigorous (1-10 x 10^{-4} Msun/yr) accretion bursts, which are intervened with longer periods (~1000 yr) of quiescent accretion. Note that bursts of mass accretion are correlated with the clump infall in the upper panel. I would like to thank Dr. Takahiro Kudoh and Dr. Sergiy Khan for the help with animation. |