Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978a%26a....64..351f&link_type=abstract
Astronomy and Astrophysics, vol. 64, no. 3, Mar. 1978, p. 351-358. Research supported by the Aerospace Corp.
Astronomy and Astrophysics
Astrophysics
9
Faculae, Line Spectra, Magnetic Flux, Solar Magnetic Field, Solar Spectra, Absorption Spectra, Magnetic Signatures
Scientific paper
It is pointed out that for any given Fraunhofer line, there should exist an entire range of facular line profiles. The consequences of the hypothesis that the structure of faculae and pores is determined to first order by the total magnetic flux is examined, and therefore, there should be a one parameter family of line profiles, with the magnetic flux being that parameter. Observations from a magnetograph are used to construct this family of line profiles in a statistical manner. Results are given for the two absorption lines, Fe I 525.022 nm and Fe I 524.706 nm. It is shown that the shape of these profiles changes continuously from the smallest to the largest faculae, even including pores. It is concluded that the T(tau) relation in faculae and pores is a strong function of the total flux, and that a generalized model of this phenomenon is needed. An additional effect of this phenomenon is that past observations of facular line profiles and continuum contrasts have probably been seriously contaminated by observational selection.
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