Relationship of magnetic field strength and brightness of fine-structure elements in the solar temperature minimum region

Details Relationship of magnetic field strength and brightness of fine-structure elements in the solar temperature minimum region Relationship of magnetic field strength and brightness of fine-structure elements in the solar temperature minimum region

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...355..719c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 355, June 1, 1990, p. 719-725. Research supported by the U.S. Navy.

Computer Science

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15

Brightness Temperature, Field Strength, Fine Structure, Solar Magnetic Field, Solar Temperature, Magnetic Flux, Solar Atmosphere, Solar Granulation, Spatial Distribution, Telescopes

Scientific paper

A quantitative relationship was determined between magnetic field strength (or magnetic flux) from photospheric magnetograph observations and the brightness temperature of solar fine-structure elements observed at 1600 A, where the predominant flux source is continuum emission from the solar temperature minimum region. A Kitt Peak magnetogram and spectroheliograph observations at 1600 A taken during a sounding rocket flight of the High Resolution Telescope and Spectrograph from December 11, 1987 were used. The statistical distributions of brightness temperature in the quiet sun at 1600 A, and absolute value of magnetic field strength in the same area were determined from these observations. Using a technique which obtains the best-fit relationship of a given functional form between these two histogram distributions, a quantitative relationship was determined between absolute value of magnetic field strength B and brightness temperature which is essentially linear from 10 to 150 G. An interpretation is suggested, in which a basal heating occurs generally, while brighter elements are produced in magnetic regions with temperature enhancements proportional to B.

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