Property and evolution of EUV and X-ray bright points in coronal holes
Abstract
It has been shown (e.g, Sattarov et al. 2002, ApJ, 564, 1042) that solar cycle variation of number of X-ray bright points (XBPs) can be caused by the visibility effect, i.e., the increased background due to scattering from bright active regions alters identification of XBPs. In contrast, the number of photospheric bipoles - the magnetic counterparts of bright points - is independent of solar cycle. On the other hand, several previous studies reported enhanced density of XBPs in coronal holes. It has also been shown that there is positive correlation between XBP number in coronal holes and solar wind density. We study magnetic and thermal properties, location and motions of EUV and X-ray bright points in coronal holes using observations from SOHO EIT (171, 195 and 304 A) and Yohkoh SXT.
- Publication:
-
34th COSPAR Scientific Assembly
- Pub Date:
- 2002
- Bibcode:
- 2002cosp...34E1152S