Solar Active Regions as a Percolation Phenomenon. II.

Details Solar Active Regions as a Percolation Phenomenon. II. Solar Active Regions as a Percolation Phenomenon. II.

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...460..522s&link_type=abstract

Astrophysical Journal v.460, p.522

Astronomy and Astrophysics

Astronomy

24

Magnetohydrodynamics: Mhd, Sun: Activity, Sun: Magnetic Fields

Scientific paper

The persistence of solar active regions was previously modeled in terms of percolation releasing magnetic flux from deep in the solar interior (Wentzel & Seiden 1992). Harvey's (1993) data on the size distribution of active regions at the end of emergence are reinterpreted in terms of a power law at small sizes and exponential at larger sizes. This combination is characteristic of percolation near the critical point. We have added a simple model for the magnetic polarity of the released loops and for their diffusion once they reach the surface. We present simulated active-region maps and size and age distributions.

Affiliated with

Also associated with

No associations

Rating

Solar Active Regions as a Percolation Phenomenon. II. 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 Active Regions as a Percolation Phenomenon. II., we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Solar Active Regions as a Percolation Phenomenon. II. will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1645057