Solar magnetic fields and convection. I - Active regions and sunspots

Details Solar magnetic fields and convection. I - Active regions and sunspots Solar magnetic fields and convection. I - Active regions and sunspots

May 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975ap%26ss..34..347p&link_type=abstract

Astrophysics and Space Science, vol. 34, May 1975, p. 347-362.

Astronomy and Astrophysics

Astrophysics

44

Astronomical Models, Convective Flow, Magnetic Flux, Solar Activity, Solar Magnetic Field, Sunspots, Dynamo Theory, H Alpha Line, Magnetohydrodynamic Stability, Solar Cycles, Solar Wind

Scientific paper

The phenomenological model of solar magnetic fields proposed differs drastically from the currently popular diffuse tangled field models. One of the major differences is that the magnetic flux concentrations seen in sunspots, in active regions, and even in quiet regions are caused by long-lived flux ropes, rather than by convective motions. These widely separated helically twisted ropes originate beneath the convection zone, and throughout their lives are impervious to supergranule and granule motions. The model is incompatible with the dynamo theory and with convection models in which formation of sunspot fields is attributed to supergranulation.

Affiliated with

Also associated with

No associations

Rating

Solar magnetic fields and convection. I - Active regions and sunspots 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 Solar magnetic fields and convection. I - Active regions and sunspots, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Solar magnetic fields and convection. I - Active regions and sunspots will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1047930