Geodesic
An instability of radiative shock wave in the presence of magnetic field
Matematičeskoe modelirovanie, Tome 22 (2010) no. 7, pp. 65-81.

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The mathematical modelling of the matter deceleration in a magnetohydrodynamics radiative shock wave was performed. The problem is relevant to classical T Tauri stars. We consider the limit where the initial deceleration and heating of plasma (at the entrance to the cooling zone) occurs in a fast magnetohydrodynamic shock wave. To calculate the intensity of radiative losses we use “real” and “power-law” radiative functions. We determine the stability/instability of the radiative shock wave as a function of parameters of the incoming flow: velocity, strength of the magnetic field, and its inclination to the surface of the star. In a number of simulation runs with the “real” radiative function, we find a simple criterion for stability of the radiative shock wave for infalling matter velocity is $1.3\cdot10^7$ cm/sec.
Keywords: accretion, radiation, shock wave, magnetohydrodynamics. 
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V. A. Gasilov; A. V. Koldoba; G. V. Ustyugova. An instability of radiative shock wave in the presence of magnetic field. Matematičeskoe modelirovanie, Tome 22 (2010) no. 7, pp. 65-81. http://geodesic.mathdoc.fr/item/MM_2010_22_7_a4/

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