Astrophysics and Space Science

, Volume 106, Issue 1, pp 1–34 | Cite as

Flare stars: Postflare behaviour of emission lines

  • G. A. Gurzadyan


The problem of the postflare behaviour of chromospheric emission lines in UV Cet-type flare stars is considered. It is shown that the postflare behaviours of different emission lines differ essentially from one another. In particular, the intensity of hydrogen and helium lines must be greatest at flare peak in continuum, while the intensities of 2800 MgII and H and K CaII lines reach their maximum magnitudes in the intermediate period between two flares. Theoretical postflare light curves are derived for the most important chromospheric lines: helium, hydrogen ionized magnesium and calcium (Figures 8, 9, 11, and 16). The definite regularities in sequence of these light curves are established (Figure 17). Methods of obtaining the mass concentration,n*, in the chromospheres of flare stars based on the analysis of hydrogen and calcium light curves are elaborated. Values ofn* obtained for a group of UV Cet-type flare stars are listed in Table VII. The conditions of the intensification of emission lines during the flare are examined, as is the possibility of the existence of an empirical relationship between chromospheric concentration,n* and flare frequency,f U .


Helium Flare Emission Line Mass Concentration Empirical Relationship 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.


  1. Brown, R. T.: 1971,Astrophys. J. 170, 387.Google Scholar
  2. Butler, C. J., Byrne, P. B., Andrews, A. D., and Doyle, J. G.: 1981,Monthly Notices Roy. Astron. Soc. 197, 815.Google Scholar
  3. Gerschberg, R. E. and Chugainov, P. F.: 1967,Astron. J. USSR 44, 260.Google Scholar
  4. Gurzadyan, G. A.: 1967,Doklady Acad. Nauk SSSR 172, 287.Google Scholar
  5. Gurzadyan, G. A.: 1969,Planetary Nebulae, Gordon and Breach, New York.Google Scholar
  6. Gurzadyan, G. A.: 1977,Astrophys. Space Sci. 52, 51.Google Scholar
  7. Gurzadyan, G. A.: 1980,Flare Stars, Pergamon Press, Oxford.Google Scholar
  8. Gurzadyan, G. A.: 1983,Astrophys. Space Sci. 91, 157.Google Scholar
  9. Gurzadyan, G. A.: 1984,Stellar Chromospheres, Nauka, Moscow, (in Russian).Google Scholar
  10. Haisch, B. M., Linsky, J. L., Bornmann, P. L., Stencel, R. E. et al.: 1983,Astrophys. J. 267, 280.Google Scholar
  11. Harrington, J. P., Lutz, J. H., Seaton, M. J. and Stickland, O. J.: 1980,Monthly Notices Roy. Astron. Soc. 191, 13.Google Scholar
  12. Mochnacki, S. W. and Schommer, R. A.: 1979,Astrophys. J. 231, L77.Google Scholar
  13. Peach, G.: 1966,Proc. Phys. Soc. 87, 381.Google Scholar
  14. Rose, J. E. and Aller, L. H.: 1976,Science 191, 1223.Google Scholar
  15. Shull, J. M. and van Stenberg, M.: 1982,Astrophys. J. Suppl. 48, 95.Google Scholar
  16. Sobolev V. V.: 1956,Transfer of Radiative Energy in the Atmospheres of Stars and Planets, Moscow, (in Russian).Google Scholar

Copyright information

© D. Reidel Publishing Company 1984

Authors and Affiliations

  • G. A. Gurzadyan
    • 1
  1. 1.Polytechnic InstituteErevanArmenian SSR, USSR

Personalised recommendations