Generalized concept of flares on late-type stars

Details Generalized concept of flares on late-type stars Generalized concept of flares on late-type stars

Oct 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26at...20..531k&link_type=abstract

Astronomical and Astrophysical Transactions, vol. 20, Issue 3, pp.531-537

Astronomy and Astrophysics

Astronomy

Stellar Activity, X-Ray Flares, Magnetic Fields

Scientific paper

Different kinds of stellar flares - very fast flares (0.1-10 s spikes), impulsive flares lasting 100-1000 s and flares with a long decay of the soft X-rays over hours-days - are described. Impulsive flares arises as a consequence of the energy input into the magnetically confined plasma. There is reason to suppose that these flares, which occur mainly on active red dwarfs (UV Cet-type), are a result of evolution of local magnetic fields, and they develop in low-lying loops. The response of the outer atmosphere of a star to impulsive heating is considered. It allows us to understand the origin of the X-ray and optical flare radiation in the framework of a uniform approach. In particular, optical radiation of sources formed during the gas-dynamic process considered does describe the flare observations quite well. Long-decay X-ray flares (LDF), which are more typical for components of RS CVn binaries, especially, for late-type subgiants, are a result of post-eruptive energy release. The duration of LDFs and peculiar features of the temporal behaviour of the temperature can be explained if this process is developed under prolonged heating in giant dense loops. The analysis of gas-dynamic processes in giant coronal loops indicates the existence of sustained heating during the soft X-ray flare. The total energy of such LDFs can reach 1035-1036 ergs, that can be supplied by large scale (global) magnetic fields.

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