Volume 385, Number 2, April II 2002
|Page(s)||511 - 516|
|Section||Interstellar and circumstellar matter|
|Published online||15 April 2002|
The complex X-ray spectrum of the supersoft source
Astronomical Institute, Utrecht University, PO Box 80000, 3508 TA Utrecht, The Netherlands
2 SRON National Institute for Space Research, Sorbonnelaan 2, CA 3584 Utrecht, The Netherlands
3 Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
4 Observatoire Astronomique, UA 1280 CNRS, 11 rue de l'Université, 67000 Strasbourg, France
Corresponding author: H. Bearda, email@example.com
Accepted: 17 January 2002
We present the X-ray spectrum of / , obtained with the Medium Energy Grating spectrometer of the Chandra X-ray Telescope. The simplest models used by earlier authors, stellar atmospheres in combination with a thermal plasma in collisional ionization equilibrium, cannot explain the spectrum. Neither does a photo-ionized plasma. We identify P Cygni profiles of Fe XVII and O VIII, from which we conclude that these lines arise in a wind. We conclude that major uncertainty exists about the bolometric luminosity of , and perhaps of supersoft sources in general, so that the theoretical prediction that this luminosity derives from steady nuclear burning cannot be verified.
Key words: stars: atmospheres / binaries: close / line: identification / stars: individual: / stars: winds, outflows / X-rays: binaries
© ESO, 2002
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.