Coronal holes and high-speed wind streams

Details Coronal holes and high-speed wind streams Coronal holes and high-speed wind streams

Aug 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977rvgsp..15..257z&link_type=abstract

Reviews of Geophysics and Space Physics, vol. 15, Aug. 1977, p. 257-269.

Astronomy and Astrophysics

Astronomy

45

Geomagnetism, M Region, Magnetic Variations, Solar Activity Effects, Solar Corona, Solar Wind, Astronomical Models, Solar Wind Velocity, Spaceborne Astronomy, Wind Profiles

Scientific paper

Coronal holes, regions of unusually low density and low temperature in the solar corona, are identified as Bartel's M regions, i.e., sources of high-speed wind streams that produce recurrent geomagnetic variations. Throughout the Skylab period the polar caps of the sun were coronal holes, and at lower latitudes the most persistent and recurrent holes were equatorial extensions of the polar caps. The holes rotated 'rigidly' at the equatorial synodic rate. They formed in regions of unipolar photospheric magnetic field, and their internal magnetic fields diverged rapidly with increasing distance from the sun. The geometry of the magnetic field in the inner corona seems to control both the physical properties of the holes and the global distribution of high-speed wind streams in the heliosphere. Phenomenological models for the birth and decay of coronal holes have been proposed.

Affiliated with

Also associated with

No associations

Rating

Coronal holes and high-speed wind streams does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Coronal holes and high-speed wind streams, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Coronal holes and high-speed wind streams will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1881375