A two-zone model of coronal hole structure in the high corona.
Abstract
The authors propose a two-zone model of coronal hole structure in the high corona at height around 1.5 to 1.7 solar radii, in which a central zone and a boundary zone can be clearly distinguished. The model is suggested by comparing the results of computation of potential magnetic fields of the corona and meter-decameter radio observations. The coronal magnetic fields were computed from the surface field observed at the John M. Wilcox Solar Observatory at Stanford University. The radio data were obtained at the Clark Lake Radio Observatory of the University of Maryland. The location of a coronal hole at the base of the corona is determined with the help of He I 10830 Å maps observed at the National Solar Observatory at Kitt Peak.
- Publication:
-
Solar and Stellar Coronal Structure and Dynamics
- Pub Date:
- 1988
- Bibcode:
- 1988sscd.conf..458W
- Keywords:
-
- Coronal Holes;
- Coronal Loops;
- Solar Magnetic Field;
- Density Distribution;
- Magnetic Field Configurations;
- Optical Thickness;
- Solar Observatories;
- Thermal Emission;
- Solar Physics;
- Solar Coronal Holes: Models;
- Solar Coronal Holes: Structure;
- Solar Coronal Holes: Radio Radiation;
- Solar Coronal Holes: Magnetic Fields