Measurements of magnetic fields in solar prominences.
Abstract
Magnetic fields can be measured, in solar prominences, by means of two different basic mechanisms that are responsible for the introduction (or the reduction) of a given amount of polarization in spectral lines: these are the Zeeman effect and the Hanle effect. Through the splitting of the magnetic components of a spectral line, the Zeeman effect is capable of introducing a certain amount of circular polarization across the line profile. The Hanle effect consist of a modification of the linear polarization that is induced in spectral lines by the anisotropic illumination of the prominence plasma by the photospheric radiation field. These two effects are briefly discussed.
- Publication:
-
NASA Conference Publication
- Pub Date:
- December 1986
- Bibcode:
- 1986NASCP2442..203L
- Keywords:
-
- Line Spectra;
- Solar Magnetic Field;
- Solar Prominences;
- Solar Wind;
- Zeeman Effect;
- Circular Polarization;
- Linear Polarization;
- Photosphere;
- Solar Physics;
- Spectrum Analysis;
- Solar Physics;
- Magnetic Fields:Solar Prominences;
- Solar Prominences:Magnetic Fields