Hostname: page-component-848d4c4894-xfwgj Total loading time: 0 Render date: 2024-06-25T16:30:50.569Z Has data issue: false hasContentIssue false
  • English
  • Français

The Balmer decrement in red dwarfs spectra during the flares and quiescent state

Published online by Cambridge University Press:  23 September 2016

M.M. Katsova
M.M. Katsova*
Affiliation:
Sternberg State Astronomical Institute, Moscow State University, 119899 Moscow V-234, U.S.S.R.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The Balmer decrements observed from flare stars during the flares and out-of-flare are analyzed on the basis of our new consideration of hydrogen atom kinetics. The steep Balmer decrements correspond to the emission source with electron density ne ≤ 1013 cm−3 optical depth at the Lα line centre τ(Lα) ≤ 107 for T=104, The low-sloping Balmer decrement, being typical for flare maximum of red dwarfs as well as for several flare stars with measurable X-ray emission out-of-flare, are described by ne = 3 · 1013–1014 cm−3 and τ(Lα)= 107 − 108 for T=(1−1, 5) · 104 K.

Type
IV Theoretical Problems and Interpretation of Observations
Information
Symposium - International Astronomical Union , Volume 137: Flare Stars in Star Clusters, Association and Solar Vicinity , 1990 , pp. 321 - 323
Copyright
Copyright © Kluwer 1990 

References

Bruevich, E.A., Livshits, M. A. this proceeding Doyle, J.G., Butler, C.J., Byrne, P.B., van den Oord, G.H.J.: 1988, Astron, Astrophys.V. 193, P.229 Google Scholar
Gershberg, R.E.: 1974a. Astron.Zhurn. of USSR, V. 51, P.552 Google Scholar
Gershberg, R.E.: 1974b. Izv.Krymsk.Astrophys.Obs., V. 51, P. 117 Google Scholar
Grinin, V.P.: 1969, Astrofizika, V. 5, P.213 Google Scholar
Katsova, M.M., Livshits, M.A.: 1988, “Activity in Cool Star Envelopes” Eds. Havnes, O. et al. Dordrecht: Kluwer D., P.143 CrossRefGoogle Scholar
Pettersen, B.R., Hawley, S.L.: 1988, Prepr. Ser. Inst. of Theor. Astrophys.Univ. of Oslo, No 005 Google Scholar