Magnetohydrodynamic Tube Waves and High Speed Solar Wind Streams
Abstract
It has been widely conjectured that magnetohydrodynamic (MHD) waves may provide the extra momentum or energy required to explain the high speed solar wind streams that originate in coronal holes. Although the magnetic structuring inherent in this problem has been incorporated into models of the bulk flow, this is not generally true of the associated treatments of wave propagation. In particular, as pointed out by Davila (1985), we might generally expect the magnetic geometry to substantially modify those waves whose wavelength is comparable to the hole width. Using both a geometrical optics and an eigenmode approach, Davila addressed the question of wave propagation in a simple uniform width flux slab model of a coronal hole and concluded the hole may act as a `leaky wave guide', i.e., waves travelling along it may leak into the surrounding corona, but
- Publication:
-
Solar Physics
- Pub Date:
- March 1987
- DOI:
- 10.1007/BF00152086
- Bibcode:
- 1987SoPh..108..183C
- Keywords:
-
- Coronal Holes;
- Magnetohydrodynamic Waves;
- Solar Wind Velocity;
- Wave Propagation;
- Cold Plasmas;
- Group Velocity;
- High Speed;
- Solar Atmosphere;
- Wave Equations;
- Solar Physics;
- Solar Wind;
- Coronal Hole;
- Fast Wave;
- Hole Model;
- Slab Model