Cooling curves of stellar flare plasmas from time resolved optical spectroscopy

Details Cooling curves of stellar flare plasmas from time resolved optical spectroscopy Cooling curves of stellar flare plasmas from time resolved optical spectroscopy

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26as...87...33h&link_type=abstract

Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 87, no. 1, Jan. 1991, p. 33-47. Research supported by CNR an

Mathematics

Logic

8

Cosmic Plasma, Electron Energy, Emission Spectra, Spectral Line Width, Stellar Flares, Stellar Composition, Stellar Models, Stellar Spectra

Scientific paper

The relative importance of the basic phenomena that drive the emission line fluxes during the stellar flares in the spectral range 3600 - 4400 A, is so far, still poorly known. This paper discusses the impact on the chromosphere of the flare soft X-ray and optical/(E)UV continuum, as well as the plasma expansion and temperature effects for emission lines. For each spectral line, models are developed, based on the main atomic processes taking place in the flare plasma which is assumed to be stationary and optically thin. This preliminary model is applied to four flares on the active dMe stars UV Ceti, Proxima Cen, and AD Leo, to investigate the cooling of the flare plasma that emits in these lines. The results provide convincing evidence that the line fluxes are largely influenced by variation in temperature. By comparing the results for diffferent spectral lines, the modeling also provides information on the line opacities of the flare medium.

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