Issue |
A&A
Volume 389, Number 1, July I 2002
|
|
---|---|---|
Page(s) | 228 - 238 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20020529 | |
Published online | 14 June 2002 |
High-resolution X-ray spectroscopy of Procyon by Chandra and XMM-Newton
1
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, a.j.j.raassen@sron.nl
Received:
27
August
2001
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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