NUMERICAL-SIMULATION OF THE CURRENT SHEET ABOVE SOLAR SPOTS

Current sheet (CS) creation in a region with an X-type zero magnetic f ield line in plasma was simulated by numerically solving the 3D MHD eq uations for conditions which were close to the solar corona: the distu rbance propagated from the photosphere boundary under which the magnet ic field sources were situated. Some of values (B, rho, V) were set on the photosphere boundary, while others were determined from the condi tions inside the region. Several Alfven times after its creation, the CS motion practically ceased, and the plasma velocity changed its dire ction above the sheet, so that the plasma flow was directed into the C S from both sides.