Volume 413, Number 2, January II 2004
|Page(s)||643 - 655|
|Section||Stellar structure and evolution|
|Published online||18 December 2003|
X-ray spectroscopy of the Hertzsprung-gap giant star 31 Com, observed with XMM-Newton*
Dipartimento di Scienze Fisiche ed Astronomiche, Sezione di Astronomia, Università di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
2 INAF – Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
3 Research and Scientific Support Department, ESA-ESTEC, Noordwijk, The Netherlands
Corresponding author: L. Scelsi, firstname.lastname@example.org
Accepted: 29 September 2003
We have analysed the XMM-Newton X-ray spectra of the yellow giant 31 Com with the aim of deriving information on the coronal structures of this archetypical Hertzsprung-gap star. To determine the emission measure distribution vs. temperature, , and the elemental abundances of the coronal plasma, with an accurate line-based approach, we have developed a new method for simple and accurate line measurements, based on rebinning and co-adding the two RGS spectra. We have reconstructed the independently with both APED and CHIANTI atomic databases in order to investigate possible differences in the final outcome of the analysis, and we have obtained consistent results. The derived emission measure distribution has a well defined peak at K and a significant amount of plasma at higher temperatures; there is also evidence for plasma at temperatures below ~106.5 K, with a mean electron density of ~ cm-3, as inferred from the line ratio of the triplet. We have made a global fitting of the EPIC spectra, using multi-component isothermal (3-T) model, and then compared the results with the , looking for a consistent multi-temperature description of both the RGS and EPIC spectra, over the whole spectral range. While the and the 3-T models individually provide a good description of the data set on which they are based, none of them describes adequately the data of all the other instruments; the disagreements may be related, at least in part, to cross-calibration problems. Finally, we have used the to derive information about the properties of the coronal structures. Our results indicate that the corona of 31 Com is dominated by a class of magnetic loops with peak temperature ~107 K and apparently more isothermal than the solar ones.
Key words: X-rays: stars / techniques: spectroscopic / stars: activity / stars: coronae / stars: individual: 31 Com
© ESO, 2004
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