Abstract
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.
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References
Pettersen, B.R., 1974, Inst. of Theor. Astrophys., Blindern, Oslo. No.46.
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.
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© 1986 Springer-Verlag
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Butler, C.J., Rodono, M. (1986). Coordinated EXOSAT and spectroscopic observations of flare stars and coronal heating. In: Zeilik, M., Gibson, D.M. (eds) Cool Stars, Stellar Systems, and the Sun. Lecture Notes in Physics, vol 254. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-16763-3_212
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DOI: https://doi.org/10.1007/3-540-16763-3_212
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