High-resolution spectroscopy of active regions. II Line-profile interpretation, applied to an emerging flux region

Details High-resolution spectroscopy of active regions. II Line-profile interpretation, applied to an emerging flux region High-resolution spectroscopy of active regions. II Line-profile interpretation, applied to an emerging flux region

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...95...15b&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 95, Jan. 1985, p. 15-36.

Physics

29

Astronomical Spectroscopy, Magnetic Flux, Solar Magnetic Field, Field Strength, High Resolution, Line Spectra, Oxygen Spectra

Scientific paper

The analysis of spectrograms of solar magnetic structures obtained with high spatial resolution in both directions of circular polarization is discussed, with application to observations of flux emergence. It is assumed that each spatial resolution element contains two atmospheric components: (1) a mean nonmagnetic photosphere and (2) an unresolved magnetic structure. Two observable spectral line parameters of the components are defined, and the derivation of magnetic structure parameters is calibrated by computer simulations in which the functional contribution of the magnetic field component, its field strength, its field inclination, and the line-of-sight velocity difference between the components are all variable. This grid of synthesized profiles served to define the uniqueness and margins of trial-and-error fits to the observed parameters. Reslts are presented for an emerging flux region. Magnetic flux was present over most of its area. The magnetic field strength outside pores was between 100 and 1700 G, and in one 'magnetic knot' it was about 1150 G. The field inclination and the fractional area cannot be determined separately, but the mean magnetic flux density was well determined: it ranged between 80 and 120 G in some patches and in the knot between 120 and 210 G. A strong downflow was found just outside a fast-growing pore.

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