Formation of the sunspot penumbra and origin of the return flux

Details Formation of the sunspot penumbra and origin of the return flux Formation of the sunspot penumbra and origin of the return flux

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997cha%26a..21..319l&link_type=abstract

Chinese Astronomy and Astrophysics, Volume 21, Issue 3, p. 319-326.

Astronomy and Astrophysics

Astrophysics

Scientific paper

Starting from the observed fact that the growth of the sunspot penumbra is accompanied by magnetic field enhancement and motion of extension we found through numerical MHD simulation, 1) that eddies are formed naturally in the convective layer of the sunspot, 2) that it is only near the surface of the sunspot that the magnetic field vector moves outward rapidly, to from eventually the observed field configuration of the penumbra, and 3) that because of rapid decrease of β above the photosphere, it is only in a photospheric layer 200 km thick where β ~ 1 that velocities of extension as small as 0.2 km/s can effectively rotate the magnetic vector, changing an approximately vertical umbral field towards the horizontal direction in a matter of hours (up to a day), and so forming the return flux configuration expected by Osherovich, clearly distinguishing the main umbral flux injected into the corona and the returning penumbral flux that begins already in the chromosphere and photosphere.

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