Semiempirical models of the photosphere of a solar activity complex.
Abstract
Continues the study of the flaring activity complex McMath 16025+16030. The physical state of the photosphere at two homologous flare locations is investigated on the basis of the analysis of the absorption line spectrum. Semiempirical models are built for flares at different stages of their evolution and for plages at the sites where flares occur. Prior to a flare and near the maximum of an Hα-flare, the upper layer at heights of about 300 - 400 km is heated by 1000 - 1500K, meanwhile a thin layer near the photosphere base has a temperature and density deficit. During a flare's principal stage, the upper layer gradually cools off, the lower inhomogeneous layers warm up, and the depression region expands. Simultaneously all inhomogeneities are observed to shift downwards. The suggestion is made that the propagation of a flare disturbance deep into the photosphere is a wave process. It is shown that the heating was stronger and extended over deeper photospheric layers at the sites of the parental flares, which had stronger X-ray emission, than at the sites of the related sympathetic flares.
- Publication:
-
Kinematics and Physics of Celestial Bodies
- Pub Date:
- 1995
- Bibcode:
- 1995KPCB...11b...7A
- Keywords:
-
- Solar Photosphere: Models;
- Solar Active Regions: Solar Flares