Recent papers on astro-ph
The Origin of Jets
DISK ACCRETION TO MAGNETIZED STARS
OSCILLATIONS OF MHD SHOCK WAVES ON THE SURFACES OF T-TAURI STARS
This work treats the matter deceleration in a magnetohydrodynamics radiative shock wave at the surface of a star.
The problem is relevant to classical T Tauri stars where infalling matter is channeled along the star’s magnetic field and stopped in the dense layers of photosphere. A significant new aspect of the present work is that the magnetic field has an arbitrary angle with respect to the normal to the star’s surface.
In this limit 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.
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.