Mass Transfer by Tidally Induced Spiral Shocks in An Accretion Disc
Numerical simulations of two-dimensional adiabatic inviscid flow in an accretion disc in a binary system or a proto-planetary system are performed using a second-order accurate implicit Roe upwind scheme. A purpose of the work is to estimate quantitatively the amount of mass accretion rate due to spiral shocks produced by a less massive component. The mass ratio of the binary system, q, is varied to see the tidal effect of the less-massive component on the formation of spiral shocks. Five cases, namely q = 0, 10-3, 10-2, 10-1, 1, are examined. In the case of q ≥ 10-2 steady spiral shocks persist until the end of the calculations, i.e. about 15–20 rotation periods. If q is as small as 10-3, i.e. the case of the Jupiter, the amplitude of the spiral waves is not very strong. On the basis of calculated mass accretion rate, we can determine an effective α parameter in the standard accretion disc model. It depends on q, and we found that 4 · 10-4 ≤ α eff ≤ 4 · 10-2 for 10-3 ≤ q ≤ 1.
KeywordsMass Flow Rate Accretion Disc Coarse Grid Fine Grid Spiral Wave
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