The birth of coronal holes

Abstract

Coronal holes (CHs) are large-scale regions of the corona with decreased density of material and temperatures. CHs are characterized by predominantly an open configuration of magnetic field lines. CHs are observed as regions of corona with decreased emission in soft X-rays, and appear simultaneously in different emission lines in distinct regions of solar atmosphere, Zirin (1988). CHs are known to be the source of the fast quasi-stationary solar wind (Nolte et al. 1976). At the same time answers to key questions which are related to the originating (the birth) of coronal holes till now are not obtained. It is known a little works in which the birth of CHs were investigated (Solodina et al. 1977; Bohlin & Sheeley 1978; Watari et al. 1995). The objective of this paper is to study the birth of non-polar CHs. This paper continues our paper Fainshtein et al. (2002), in which one the birth of coronal holes was studied.To search for other articles by the author(s) go to: