The common observation that where photospheric magnetic fields are strong, the overlying corona is bright is examined quantitatively. White light coronal brightness is employed because it is independent of coronal temperature and is directly related to coronal electron density. Brightness data for t
Photospheric Magnetic Fields on March 7, 1970
โ Scribed by LIVINGSTON, W.; HARVEY, J.; SLAUGHTER, C.
- Book ID
- 109672092
- Publisher
- Nature Publishing Group
- Year
- 1970
- Tongue
- English
- Weight
- 636 KB
- Volume
- 226
- Category
- Article
- ISSN
- 0028-0836
No coin nor oath required. For personal study only.
๐ SIMILAR VOLUMES
The effects of line profile variations, due to the temperature enhancements connected with photospheric magnetographic measurements are evaluated in a quantitative way: taking into account these results, the differences found by many au.thors between the values of the field obtained with different F
We consider proposed mechanisms for the formation of coronal holes, and identify as crucial the issue whether the holes are permeated by rigidly rotating fields. It is suggested that the interaction between such a field and the differentially rotating, diffusive solar envelope will produce a fore af