Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...296..268r&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 296, Sept. 1, 1985, p. 268-277.
Astronomy and Astrophysics
Astrophysics
15
Circular Polarization, Magnetic Flux, Magnetohydrodynamics, Photosphere, Solar Magnetic Field, Stokes Law Of Radiation, Bernoulli Theorem, Steady Flow, Thermodynamic Properties, Zeeman Effect
Scientific paper
Dynamic models of flux tubes were used to interpret the presence of mass motions with large velocity gradients associated with spatially unresolved magnetic elements in the solar photosphere. A downflow was necessary in order to concentrate the magnetic field and provide a heating mechanism to brighten the flux tubes. There are two types of steady flow models: one has a moderate field strength (less than 1 kG) and a downflow decelerating with increasing depth and the second has a strong field and a downflow accelerating with increasing depth. To distinguish between these two field strengths, observed line profiles were compared to calculated line profiles. The comparison revealed that the main properties of the intensity line profiles and asymmetries of Stokes V-profiles was best explained by magnetic elements with moderate field strength. Further study is necessary to determine the reason for the redshift of the V-zero crossing point.
Cheng Fang
Rees David E.
Ribes Elizabeth
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