The polarization of metre-wave solar emission
Abstract
Differences in theory and observation for U-bursts and bipolar Type I storms are noted. Several simple closed-loop magnetic field configurations are considered, and the conditions are derived which are necessary to produce polarization reversals as a function of frequency and viewing angle. Generally, three stages (unipolar, bipolar and another, but in an opposite sense, unipolar) are expected to be observed while the source traverses the solar disk from the east limb to the west limb. The calculations are applied to the observed positions of several bipolar Type I sources, and an upper limit of the magnetic field strength is deduced as about 1 to 1.5 G at R = 1.5 solar radii
- Publication:
-
Publications of the Astronomical Society of Australia
- Pub Date:
- 1980
- DOI:
- 10.1017/S1323358000018786
- Bibcode:
- 1980PASA....4...56S
- Keywords:
-
- Polarized Radiation;
- Radio Sources (Astronomy);
- Solar Activity;
- Solar Magnetic Field;
- Solar Radiation;
- Solar Radio Bursts;
- Bipolarity;
- Magnetic Dipoles;
- Solar Corona;
- Sunspots;
- Solar Physics