Hostname: page-component-6bf8c574d5-t27h7 Total loading time: 0 Render date: 2025-02-23T06:08:56.223Z Has data issue: false hasContentIssue false
  • English
  • Français

The Fine Temporal Structure of The EV Lacertae Flare on February 6, 1986 at the C IV (λl550 Å) Resonance Line II. Interpretation

Published online by Cambridge University Press:  27 September 2017

M.M. Katsova  and
M.A. Livshits
M.M. Katsova
Affiliation:
Sternberg State Astronomical Institute, University of Moscow, 119899 Moscow, USSR
M.A. Livshits
Affiliation:
Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, Academy of Sciences Troitsk, 142092 Moscow Region, USSR

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.

Flare optical continuum with duration above one minute is emitted by a gas condensation with T ≈ 104 K, which may form in a gas-dynamic process. The light carve slope implies that this flare consists of several elementary events. The features of the initial C IV line burst during one elementary event are determined by numerical simulation. The comparison of theoretical intensity and duration of the C IV burst with the observations of the EV Lac flare on February 6, 1986 shows that the observed elementary event in the C IV line is consistent with the formation of a radiative shock wave with an explosive evaporation of the chromosphere. The possibility of the appearance of C IV doublet emission, accompanying the entire process, is also discussed.

Type
Session I: Stellar Flares
Information
International Astronomical Union Colloquium , Volume 104 , Issue 2: Solar and Stellar Flares , 1989 , pp. 71 - 74
Copyright
Copyright © Kluwer 1989

References

Burnasheva, B.A., Gershberg, R.E., Zvereva, A.M., Ilyin, I.V., Shakhovskaya, N.I., Sheikhet, A.I.: 1988, Astron. Journ. of USSR. 65 (Paper I).Google Scholar
Fisher, G.H.: 1986, in Radiation Hydrodynamics, Mihalas, D., Winkler, K.-H.A. (eds), Springer-Verlag, p. 53.Google Scholar
Gershberg, R.E.,, Petrova, P.P.: 1986, in “Flare stars and related objects”, Mirzoyan, L.V. (ed), Erevan, Publ. Ac. Sci. Armenian SSR, p. 38.Google Scholar
Ivanov, V.V.: 1973. Transfer of Radiation in Spectral Lines. Washington. U.S. Cov. Print. Office.Google Scholar
Katnova, M.M.: 1982, Astron. Journ. of USSR 59, 1124.Google Scholar
Katsova, M.M., Kosovichev, A.G.: 1981, Astrofizika 17, 285.Google Scholar
Katsova, M.M., Livshits, M.A.: 1983, in “Activity in Red-Dwarf Stars”, Byrne, P.B., Rodonò, M. (eds), Reidel Pubbl.Co., p. 617.Google Scholar
Katsova, M.M., Livshits, M.A.: 1987, in “Solar Maximum Analysis. II”, Stepanov, V.E., Obridko, V.N. (eds), Irkutsk.Google Scholar
Katsova, M.M., Livshits, M.A.: 1988, in “Activity in Cool Stars Envelopes”, Havnes, O., Pettersen, B., Schmidt, J.H.M.M., Solheim, J.E. (eds.), D.Kluwer Acad. Publ., p. 143.Google Scholar
Kostyuk, N.D., Pikel'ner, S.B.: 1974, Astron. Journ. of USSR 51, 1002.Google Scholar
Livshits, M.O., Badalyan, O.G., Kosovichev, A.G., Katsova, M.M.: 1981, Solar Phys. 73, 269.Google Scholar
Naghirner, D.I.: 1975, Proc. of Astron. Observ., Univ. of Leningrad. Vol. 31, p. 3.Google Scholar