Volume 389, Number 1, July I 2002
|Page(s)||228 - 238|
|Section||Stellar structure and evolution|
|Published online||14 June 2002|
High-resolution X-ray spectroscopy of Procyon by Chandra and XMM-Newton
SRON National Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
2 Astronomical Institute “Anton Pannekoek”, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
3 Paul Scherrer Institut, Würenlingen & Villigen, 5232 Villigen PSI, Switzerland
4 Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA
5 Mullard Space Science Laboratory, University College London, Surrey, RH5 6NT, UK
6 Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
Corresponding author: A. J. J. Raassen, firstname.lastname@example.org
Accepted: 5 April 2002
We report the analysis of the high-resolution soft X-ray spectrum of the nearby F-type star Procyon in the wavelength range from 5 to 175 Å obtained with the Low Energy Transmission Grating Spectrometer (LETGS) on board Chandra and with the Reflection Grating Spectrometers (RGS) and the EPIC-MOS CCD spectrometers on board XMM-Newton. Line fluxes have been measured separately for the RGS and LETGS. Spectra have been fitted globally to obtain self-consistent temperatures, emission measures, and abundances. The total volume emission measure is cm-3 with a peak between 1 and 3 MK. No indications for a dominant hot component ( MK) were found. We present additional evidence for the lack of a solar-type FIP-effect, confirming earlier EUVE results.
Key words: stars: individual: Procyon, α Canis Minoris / stars: coronae / stars: late-type / stars: activity / X-rays: stars
© ESO, 2002
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