Preprint Logo P104 November
2005


To be published in:
JENAM2005 Proceedings

CPD-41°7742: an unusual wind interaction+

H. Sana1,*, E. Gosset1,**, G. Rauw1,**, E. Antokhina2, P. Royer3, J. Manfroid1,*** and J.-M. Vreux1


1 Institut d'Astrophysique et de Géophysique - Université de Liège, Allée du 6 Août, Bât B5c, B-4000 Liège (Sart Tilman), Belgium
2 Sternberg Astronomical Institute, Moscow State University, Universitetskii Pr., 13, 119899 Moscow, Russia
3 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, 3001 Leuven, Belgium

* Research Fellow FNRS, Belgium
** Research Associate FNRS, Belgium
*** Research Director FNRS, Belgium

+ Based on observations collected at the European Southern Observatory (La Silla, Chile) and with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member states and the USA (NASA).


Abstract

     We summarize the results of a multiwavelength observing campaign on the massive eclipsing binary CPD-41°7742, another remarkable object in the young open cluster NGC 6231. Our campaign relies on high resolution echelle spectroscopy, narrow-band optical photometry, and XMM-Newton X-ray observations. Combined with the spectroscopic analysis, the light curve analysis provides a direct measurement of the masses and sizes of the system components. However, the most outstanding results come from the XMM-Newton observations. Our 180 ks campaign towards NGC 6231, and CPD-41°7742, provides an unprecedented phase coverage of such a close early-type binary. The EPIC-MOS light curves almost fully cover the 2.4 day period of the system and the brightness of the object is sufficient to yield a time resolution as tight as 1 ks. The X-ray flux presents clear variations along the orbit, that we interpret as the signature of an unusual wind interaction. We indeed expect that, in this O+B system, the dominant primary wind crashes into the secondary surface, leading to a wind-photosphere interaction. As a strong support to our interpretation, we provide a geometrical model that associates an extra X-ray emission to the secondary inner surface. Though quite simple, the present model matches the main features of the X-ray ligh curve.

Files
Article: jenam_cpd7742.pdf (157387 bytes): HTTP FTP (ftp://vela.astro.ulg.ac.be/preprints/)


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