Modelling the moustache phenomenon in network regions

Details Modelling the moustache phenomenon in network regions Modelling the moustache phenomenon in network regions

Nov 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...251..675s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 251, no. 2, Nov. 1991, p. 675-679.

Physics

10

Absorption Spectra, Line Spectra, Mathematical Models, Solar Physics, Solar Spectra, Faculae, Iron, Magnesium, Solar Limb, Solar Magnetic Field

Scientific paper

The intensity enhancement in the inner line wings (moustache) of Mgb1 5183 and Fe 5434.5 A observed in Ca(+) K bright points outside active regions is found to result from a superposition of a hot component (representing the magnetic structure) surrounded by a cool (intergranular) region. The I + V and I - V profiles of the magnetically sensitive line Fe 6302.5, observed strictly simultaneously with Mgb1, are equally well modeled by the same procedure (which in an earlier paper had successfully been used to explain the gap effect of Zeeman insensitive lines in plages). The Mgb1 moustaches are cospatial with the simultaneously observed Fe 6302.5 gaps. Their equal spatial extent indicates equal width of the temperature and the magnetic structures of the Ca(+) K region.

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