| Issue |
A&A
Volume 538, February 2012
|
|
|---|---|---|
| Article Number | A22 | |
| Number of page(s) | 9 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/201117387 | |
| Published online | 27 January 2012 | |
A detailed X-ray investigation of ζ Puppis
I. The dataset and some preliminary results⋆,⋆⋆
1 GAPHE, Département AGO, Université de Liège, Allée du 6 Août 17, Bât. B5C, 4000 Liège, Belgium
e-mail: naze@astro.ulg.ac.be
2 Departamento de Astronomia, Universidad de Guanajuato, Apdo Postal 144, Guanajuato, GTO, Mexico
Received: 1 June 2011
Accepted: 1 December 2011
Aims. One of the closest and brightest massive stars, ζ Puppis, was the first early-type object observed by the current generation of X-ray observatories. These observations provided some surprising results, partly confirming the theoretical predictions while simultaneously unveiling some problematic mismatches with expectations. In this series of papers, we perform a thorough study of ζ Puppis in X-rays, using a decade of XMM-Newton observations.
Methods. The star ζ Puppis was observed 18 times by XMM-Newton, totaling 1 Ms in exposure. This provides the highest quality high-resolution X-ray spectrum of a massive star to date, as well as a perfect dataset for studying X-ray variability in an “archetype” object.
Results. This first paper reports on the data reduction of this unique dataset and provides a few preliminary results. On the one hand, analysis of EPIC low-resolution spectra shows the star to have a remarkably stable X-ray emission from one observation to the next. On the other hand, fitting by a wind model of individual line profiles recorded by RGS confirms the wavelength dependence of the line morphology.
Key words: X-rays: stars / stars: early-type / stars: individual:ζPuppis / stars: mass-loss
Based on observations collected with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and the USA (NASA).
Table 1 is available in electronic form at http://www.aanda.org
© ESO, 2012
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