Magnetic-Field Structure of the Photospheric Network
Abstract
A method is developed to determine the physical parameters of the spatially unresolved photospheric network. The apparent magnetic fluxes are recorded simultaneously in the two FeI lines 5250 and 5247 Å, which belong to the same multiplet and have practically the same oscillator strength and excitation potential of the lower level, but differ in the effective Lande factor. By analysing magnetograph recordings in this pair of lines together with simultaneous recordings in the two FeI lines 5250 and 5233 Å, it is possible to separate the effects on the line profiles due to Zeeman splitting and temperature enhancement in the network.
- Publication:
-
Solar Physics
- Pub Date:
- September 1973
- DOI:
- 10.1007/BF00152728
- Bibcode:
- 1973SoPh...32...41S
- Keywords:
-
- Field Strength;
- Physical Parameter;
- Magnetic Flux;
- Characteristic Size;
- Oscillator Strength