Relationship between coronal holes, high-velocity streams and the sector structure of the interplanetary magnetic field.
Abstract
A statistical analysis of a large volume of data shows that most high-speed streams of the solar wind are generated right after passage through the sector structure (SS) of the IMF and just before passage through the coronal-hole (CH) boundary. About 74 to 87 percent of the CH is located within sectors of the same polarity, and the width of the boundary zone between the SS and CH commencement amounts to 20-40 heliographic degrees. About 38-57 percent of all high-speed streams connected with CHs commence in this zone.
- Publication:
-
Geomagnetism and Aeronomy
- Pub Date:
- April 1987
- Bibcode:
- 1987Ge&Ae..27..197O
- Keywords:
-
- Coronal Holes;
- Interplanetary Magnetic Fields;
- Magnetic Disturbances;
- Magnetohydrodynamic Flow;
- Solar Wind;
- High Speed;
- Histograms;
- Statistical Analysis;
- Interplanetary Magnetic Field:Sector Structure;
- Interplanetary Magnetic Field:Solar Coronal Holes;
- Solar Coronal Holes:Interplanetary Magnetic Field