Fast-mode magnetohydrodynamic waves in coronal holes and the solar wind

Journal Article · Tue May 01 04:00:00 EDT 1984 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/162003· OSTI ID:6593378

Fla, T; Habbal, S R; Holzer, T E; Leer, E

Fast-mode MHD waves in the solar corona can propagate in any direction relative to the background magnetic field. In coronal holes, they refract into regions of low Alfven speed and are relatively difficult to damp. These characteristics lead to the possibility that fast-mode waves transport energy from magnetically closed coronal regions into coronal holes, that they are refracted into the central retions of coronal holes, and that they deposit most of their energy in the regions of supersonic flow of high-speed solar wind streamd emanating from coronal holes. To investigate whether this possibility might be realized and fast-mode waves might play a significant role in driving high-speed streams, a parameter study is carried out to examine the propagation and damping of fast-mode waves in various coronal hole models. This study indicates a broad range of coronal hole parameters for which fast-mode waves can play such a role and emphasizes the need for an improved knowledge of large-scale coronal magnetic structure, which is required before any firm conclusions can be drawn.

• Research Organization: The Auroral Observatory, University of Tromso
• OSTI ID: 6593378
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 280:1; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
DAMPING
FLUID FLOW
FLUID MECHANICS
HYDRODYNAMICS
HYDROMAGNETIC WAVES
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
MATHEMATICAL MODELS
MECHANICS
PLASMA
SOLAR ACTIVITY
SOLAR CORONA
SOLAR WIND
STAR MODELS
STELLAR ATMOSPHERES
STELLAR CORONAE
SUPERSONIC FLOW
WAVE PROPAGATION