Chromospheric Evershed flow

doi:10.1051/0004-6361:20030385

2003-05-23

A. A. Georgakilas

E. B. Christopoulou

Athanassios Skodras

DOI：10.1051/0004-6361:20030385

原文链接

原文求助

摘要

En 中文

We studied the chromospheric Evershed flow from filtergrams obtained at nine wavelengths along the Halpha profile. We computed line-of-sight velocities based on Becker's cloud model and we determined the components of the flow velocity vector as a function of distance from the center of the sunspot, assuming an axial symmetry of both the spot and the flow. We found that the flow velocity decreases with decreasing height and that the maximum of the velocity shifts towards the inner penumbral boundary. The flow related to some fibrils deviates significantly from the average Evershed flow. The profile of the magnitude of the flow velocity as a function of distance from the spot center, indicates that the velocity attains its maximum value in the downstream part of the flow channels ( assumed to have the form of a loop). This behavior can be understood in terms of a critical flow that pass from subsonic to supersonic near the apex of the loop, attains its higher velocity at the downstream part of the loop and finally relaxes to subsonic through a tube shock. We computed the average flow vector from segmented line-of-sight velocity maps, excluding bright or dark fibrils alternatively. We found that the radial component of the velocity does not show a significant difference, but the magnitude of the vertical component of the velocity related to dark fibrils is higher than that related to bright fibrils.

Keyword:

Sun : sunspots

Sun : chromosphere

magnetohydrodynamics (MHD)

techniques : image processing