Protostars and Planets VI, Heidelberg, July 15-20, 2013
COMPUTER SIMULATION OF DUST GROWTH IN MASSIVE CIRCUMSTELLAR DISKS
Markelova, Tamara (Boreskov Institute of Catalysis SB RAS, Novosibirsk State University)
Snytnikov, Valeriy (Boreskov Institute of Catalysis SB RAS, Novosibirsk State University)
In the frame of solving problem of abiogenous synthesis matter in solar system, one of the most important problems is forming of bodies with radii longer 100 km. According to the astrocatalysis hypothesis carbohydrates are synthesized on the surface of the dust particles in the circumstellar protoplanetary disk, which provide coagulation of these particles, and therefore bodies with radii 1-10 m appear. There is problem of principle mechanism of forming of 100-km-sized bodies, as meter-sized bodies are destroyed due to collisions when they are moving with orbital velocities. There is a collisionless mechanism for solving this problem. The main point of it lies in possibility of appearance of gravitational instability in two-phase gas-dust environment. The probability depends on average particles mass. Thus it is necessary to study the influence of particles growth on increasing of the gravitational instability. One of the most suitable instruments for studying evolution of the protoplanetary disk is mathematical modeling with numerical supercomputer experiments. Numerical model was developed with primary particle motion in the equatorial plane of the disk. The model describes gas dynamics and particle motion including coagulation process. Since the numerical algorithm is based on splitting method. It was made investigation of the influence of the coagulation rate on dynamics of gas-dust system for the initial conditions in which gravitational instability appeared. It was found that coagulation rate can increase the instability rate. For some parameters it can significantly influence on the structure of the disk.
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