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A gas-dynamic model for a flare on YZ CMi: Interpretation of spectroscopic observations with high temporal resolution

Published online by Cambridge University Press:  27 September 2017

M.M. Katsova ,
M.A. Livshits ,
C.J. Butler  and
J.G. Doyle
M.M. Katsova
Affiliation:
Sternberg State Astronomical Institute, University of Moscow, 119899 Moscow, USSR
M.A. Livshits
Affiliation:
Institute of Terrestial Magnetism, Ionosphere and Radio Wave Propagation, Academy of Sciences, Troitsk, 142092 Moscow Region, USSR
C.J. Butler
Affiliation:
Armagh Observatory, College Hill, Armagh, N. Ireland
J.G. Doyle
Affiliation:
Armagh Observatory, College Hill, Armagh, N. Ireland

Abstract

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The spectra of a flare on YZ CMi, obtained with a temporal resolution of 60 seconds on March 4 1985 and over the range 3600-4400 A, are analysed using a gas-dynamic model. In this model, the optical radiation in the U-band, outside of flare maximum, is produced by a condensation formed during the gas-dynamic process. With the optical continuum described by a Planck function for a temperature of T ≈ 104K, the emitting source area S ≥ 5 10l7cm2. The hydrogen plasma kinetics of an “8 levels plus continuum” model atom are calculated, and it is shown that the low slope of the Balmer decrement, just after the flare maximum, is connected with a large population in the second level of the hydrogen atom.

Type
Session I: Stellar Flares
Information
International Astronomical Union Colloquium , Volume 104 , Issue 2: Solar and Stellar Flares , 1989 , pp. 87 - 90
Copyright
Copyright © Kluwer 1989

References

Butler, C.J., Doyle, J.G., Foing, B.H. and Rodono, M.: 1988, ‘Activity in cool star envelopes’ O., Havnes, B.R., Pettersen, J.H.M.M., Schmitt, J.E., Solheim (eds), Kluwer, p 167 CrossRefGoogle Scholar
Doyle, J.G., Butler, C.J., Byrne, P.B. and Van den Oord, G.H.J.: 1988, Astron. and Astrophys. 193, 329 Google Scholar
Fisher, G.H.: 1986, ‘Radiative Hydrodynamics’ Springer-Verlag, p 53 Google Scholar
Gershberg, R.E., Schnoll, E.E.: 1974, Izv. Krymsk. Astrophys. Observ. 50, p 122 Google Scholar
Katsova, M.M., Kosovichev, A.G., Livshits, M.A.: 1981, Astrofizika, 17, p 285 Google Scholar
Katsova, M.M., Livshits, M.A.:1988, ‘Activity in cool star envelopes’ O., Havnes, B.R., Pettersen, J.H.M.M., Schmitt, J.E., Solheim (eds) Kluwer, p 143 Google Scholar
Kostyuk, N.D., Pikel'ner, S.B.: 1974, Astron. J. of USSR, 51, p 1002 Google Scholar
Livshits, M.A., Badalyan, O.G., Kosovichev, A.G., Katsova, M.M.: 1981, Solar Phys. 73, p 269 CrossRefGoogle Scholar
Rodono, M.: 1987, private comm. Google Scholar
Sobolev, V.V.: 1960, ‘Moving envelopes of stars’ Harvard Univ. Press Google Scholar