Coordinated EXOSAT and spectroscopic observations of flare stars and coronal heating

  • C. J. Butler
  • M. Rodono
Sesssion III. Small Scale Atmospheric Structures: Data
Part of the Lecture Notes in Physics book series (LNP, volume 254)


We present some preliminary results of simultaneous monitoring of the two flare stars, UV Ceti and EQ Peg with EXOSAT and ground based optical spectro-scopy. A strong correlation, found between the Hγ emission and the soft X-ray flux, over several hours of observation of UV Ceti, suggests that much of the low level X-ray flux which has previously been considered ‘quiescent’, in fact derives from small flare events. The implication is that coronal heating in M type dwarfs may result directly from the frequent occurrence of micro-flares.


Coronal Heating Balmer Line Flare Star European Southern Observatory Balmer Line Emission 
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  1. Pettersen, B.R., 1974, Inst. of Theor. Astrophys., Blindern, Oslo. No.46.Google Scholar
  2. Rodono, M., Foing, R.H., Linsky, J.L., Butler, C.J., Haisch, B.M., Gary, D.E. and Gibson, D.M. 1985, ‘The Messenger’ ESO Bulletin No.39, 9–1O.Google Scholar

Copyright information

© Springer-Verlag 1986

Authors and Affiliations

  • C. J. Butler
    • 1
  • M. Rodono
    • 2
  1. 1.Armagh ObservatoryN. Ireland
  2. 2.Institute of AstronomyUniversity of CataniaItaly

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