Element Abundances in Stellar Coronae

J.J. Drake, J.M. Laming (1), K.G. Widing (2)

1) Code 7674L NRL, Washigton, D.C. 20375
2) Code 7674 W, Naval Research Laboratory, 4555 Overlook Ave. SW., Washington, DC 20375-5000

To appear in Proceedings of IAU Colloquium 153, Magnetodynamic Phenomena in the Solar Atmosphere: Prototypes of Stellar Activity, Makuhari, Japan, May 22-26, 1995

Abstract

About two years ago, the intrigue of the solar "FIP Effect" -- that coronal abundances of elements with a low FIP (~< 10 eV; e.g Fe, Mg, Si, Ca) are observed to be enhanced relative to those of high FIP elements (~> 10 eV; e.g. O, Ne, S; see e.g., the review by Meyer 1993) -- prompted us to study stellar coronal abundances based on new EUV spectra obtained with the Extreme Ultraviolet Explorer (EUVE). Our results to-date indicate that some stars appear to show a solar-like FIP Effect, whereas others do not (Drake et al., 1995abc; Laming et al., 1995ab).

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