[Previous] | [Session 42] | [Next]
J.J. Drake, N.S. Brickhouse, V. Kashyap, R. Smith, B. Wargelin (Harvard-Smithsonian Center for Astrophysics), J.M. Laming (Naval Research Laboratory), D.P. Huenemoerder (Massachusetts Institute of Technology Center for Space Research)
Chandra HETG spectra of the tidally interacting RS~CVn-type binary HR~1099 (V711 Tau) have been analysed in order to investigate the abundances of elements in the coronae of the system. Analogous to the results of previous studies based on EUVE and ASCA observations, the high resolution X-ray spectrum is characterised by a general paucity of metals relative to the solar photosphere, but perhaps simply reflects the underlying stellar photospheric metallicity. The most striking feature of the spectrum, however, is the very strong Ly-\alpha feature in H-like Ne. The only plausible explanation for the strength of the Ne lines is that the abundance of Ne in the coronae of HR~1099 is strongly enhanced relative to that of Fe, as compared to the solar (photospheric) mixture. We discuss the implications of this result in the context of stellar coronae and coronal abundances anomalies, draw attention to possible solar coronal analogies to the phenomena, and suggest possible reasons for the Ne enhancement.
JJD, NSB, VK, BW and RS were supported by Chandra X-ray Center~ NASA contract NAS8-39073.