Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989soph..121..299p&link_type=abstract
(IAU, Colloquium on Solar and Stellar Flares, 104th, Stanford, CA, Aug. 15-19, 1988) Solar Physics (ISSN 0038-0938), vol. 121, n
Astronomy and Astrophysics
Astronomy
43
Flare Stars, Hertzsprung-Russell Diagram, Stellar Flares, Main Sequence Stars, Ultraviolet Astronomy, X Ray Sources
Scientific paper
The flaring activity of stars across the HR-diagram is reviewed. Brightenings have been reported along the entire Main Sequence and in many stars off the Main Sequence. Some stars are decidedly young, others are in advanced stages of stellar evolution. Flares are common on stars with outer convection zones and outbursts have been reported also on other types of stars, although confirmations are needed for some of them. Recent solar results, where the occurrence rate for flares is found to exhibit a periodicity of 152 days, suggest that stellar flare data should be reanalyzed over long time baselines to see if the present confusing situation can be resolved. The radiation from stellar flares is dominated by continuum emission and about equal amounts of energy have been recorded in the optical, UV, and X-ray regions of the spectrum. In solar flares strong continuum emission is rarely recorded and a large collection of bright emission lines takes prominence. Small flares occur more frequently than large ones and the latter have longer time-scales. Flare energies can exceed 10 to the 37th erg. The most productive flare stars are those where the convective envelopes occupy large volumes. Slow stellar rotation rates are believed to reduce the level when the star has been braked significantly from its young rotation rate.
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