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Some evidence on the evolution of the flare mechanism in dwarf stars
Skumanich, Andrew
AA(High Altitude Observatory, Boulder, CO)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 309, Oct. 15, 1986, p. 858-863. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Dwarf Stars, Solar Flares, Stellar Evolution, Stellar Flares, Energy Dissipation, Late Stars, M Stars, Magnetic Stars, Solar Corona, Solar X-Rays
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White-light flare parameters are estimated for the sun as a star. It is found that these parameters fall in the same domain as those for the dMe flare stars. In particular, it is found that the time-averaged flare power loss and quiescent coronal soft X-ray power loss at solar maximum satisfies the recently proposed flare power-coronal X-ray relation for dMe stars (Doyle and Butler; Skumanich). In addition, one finds that dM stars, which are believed to be magnetically evolved dMe stars, also satisfy the same relation. On this basis, an evolutionary scenario is suggested for the flare mechanism in which the total flare rate remains, more or less, constant but the mean flare yield decreases linearly with coronal X-ray strength. It is also suggested that the flare mechanism is universal in all magnetically active dwarfs.

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