Spectral analysis of the optical continuum in the 24 April 1981 flare

Details Spectral analysis of the optical continuum in the 24 April 1981 flare Spectral analysis of the optical continuum in the 24 April 1981 flare

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...85..285n&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 85, June 1983, p. 285-302.

Physics

26

Balmer Series, Solar Flares, Solar Spectra, Spectrum Analysis, Brightness, Electron Density (Concentration), Opacity, Solar Temperature

Scientific paper

Observations of the white-light flare (WLF) of April 24, 1981 made with the multiband polarimeter at Sacramento Peak Observatory and with the Universal Spectrograph (covering 3550-9100 A) are reported and analyzed, with comparisons to data on other WLF, in terms of the peak-intensity optical continuum (below 4000 A). The spectrograph slit was positioned 3 arecsec east of the brightest point in the kernel of the flare, but outside the sunspot penumbra. The flare emission is unpolarized and characterized by broad, intense Balmer lines and a Balmer continuum superimposed over a weaker continuum attributed to H(-) emission at a height of 200-300 km. Intensity at 3600 A is 360 pct greater than that of the background solar surface, with a continuum-emitting-layer temperature of about 6700 K. Other parameters estimated include electron density = 5.3 x 10 to the 13th/cu cm, second-level H-column density = 1.1 x 10 to the 16th/sq cm, peak radiative output integrated over wavelength = 6.1 x 10 to the 27th erg/sec, and energy loss rate (at 300-km height) = 10 to the 3rd erg/sec cu cm.

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