Issue |
A&A
Volume 407, Number 1, August III 2003
|
|
---|---|---|
Page(s) | 347 - 358 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20030880 | |
Published online | 17 November 2003 |
Are stellar coronae optically thin in X-rays?
A systematic investigation of opacity effects
1
Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
2
Columbia Astrophysics Laboratory, 550 West 120th Street, New York, NY 10027, USA
3
Paul Scherrer Institut, Würenlingen & Villigen, 5232 Villigen PSI, Switzerland
4
National Institute for Space Research (SRON), Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
Corresponding author: J.-U. Ness, jness@hs.uni-hamburg.de
Received:
23
January
2003
Accepted:
2
June
2003
The relevance of resonant scattering in the solar corona has always been
discussed controversially. Ratios of emission lines from identical ions but
different oscillator strengths have been used in order to estimate damping of
resonance lines due to possible resonant scattering, i.e., absorption by
photo-excitation and re-emission out of the line of sight. The analysis of
stellar spectra in analogy to previous works for the Sun is possible now with
XMM-Newton and Chandra grating spectra and requires this issue
to be considered again. In this work we present a sample of 45 X-ray spectra
obtained for 26 stellar coronae with the RGS on board XMM-Newton and the LETGS
and HETGS on board Chandra. We use ratios of the Fe xvii lines at 15.27 Å and 16.78 Å lines to the resonance line at 15.03 Å as well
as the He-like ratio of O vii and Ne ix to measure optical
depth effects and compare them with ratios obtained from optically thin plasma
atomic databases such as MEKAL, Chianti, and APEC. From the Fe xvii line
ratios we find no convincing proof for resonance line scattering. Optical
depths are basically identical for all kinds of stellar coronae and we conclude
that identical optical depths are more probable when effects from resonant
scattering are generally negligible. The 15.27/15.03 Å ratio shows a
regular trend suggesting blending of the 15.27 Å line by a cooler Fe line,
possibly Fe xvi. The He-like
ratios for O and Ne show no indication
for significant damping of the resonance lines.
We mainly attribute deviations from the atomic databases to still uncertain
emissivities which do not agree well with laboratory measurements and which come
out with differing results when accounting for one or the other side effect.
We attribute the discrepancies in the solar data to geometrical effects from
observing individual emitting regions in the solar corona but only overall
emission for stellar coronae including photons eventually scattered into the
line of sight.
Key words: stars: activity / stars: coronae / stars: late type / X-rays: stars / atomic processes
© ESO, 2003
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