Solar magnetic field studies using the 12 micron emission lines. I - Quiet sun time series and sunspot slices

Details Solar magnetic field studies using the 12 micron emission lines. I - Quiet sun time series and sunspot slices Solar magnetic field studies using the 12 micron emission lines. I - Quiet sun time series and sunspot slices

Oct 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...333..978d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 333, Oct. 15, 1988, p. 978-995. NASA-supported research.

Astronomy and Astrophysics

Astrophysics

60

Emission Spectra, Infrared Spectra, Line Spectra, Solar Magnetic Field, Sunspots, Zeeman Effect, Fourier Transformation, H Alpha Line, Solar Atmosphere, Solar Interior, Solar Limb

Scientific paper

The use of the extremely Zeeman-sensitive IR emission line Mg I, at 12.32 microns, to study solar magnetic fields. Time series observations of the line in the quiet sun were obtained in order to determine the response time of the line to the five-minute oscillations. Based upon the velocity amplitude and average period measured in the line, it is concluded that it is formed in the temperature minimum region. The magnetic structure of sunspots is investigated by stepping a small field of view in linear 'slices' through the spots. The region of penumbral line formation does not show the Evershed outflow common in photospheric lines. The line intensity is a factor of two greater in sunspot penumbrae than in the photosphere, and at the limb the penumbral emission begins to depart from optical thinness, the line source function increasing with height. For a spot near disk center, the radial decrease in absolute magnetic field strength is steeper than the generally accepted dependence.

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