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On the perspectives of using XMM to study fundamental parameters of early-type stars

Published online by Cambridge University Press:  25 May 2016

Gregor Rauw ,
Karel A. van der Hucht ,
Rolf Mewe ,
Manuel Güdel ,
Jean-Marie Vreux ,
Eric Gosset ,
Werner Schmutz  and
Ian R. Stevens
Gregor Rauw
Affiliation:
Institut d'Astrophysique et de Géophysique, Liège, Belgium At the Fonds National de la Recherche Scientifique, Belgium
Karel A. van der Hucht
Affiliation:
Space Research Organization Netherlands, Utrecht, the Netherlands
Rolf Mewe
Affiliation:
Space Research Organization Netherlands, Utrecht, the Netherlands
Manuel Güdel
Affiliation:
ETHZ, Paul Scherrer Institute, Villingen, Switzerland
Jean-Marie Vreux
Affiliation:
Institut d'Astrophysique et de Géophysique, Liège, Belgium
Eric Gosset
Affiliation:
Institut d'Astrophysique et de Géophysique, Liège, Belgium At the Fonds National de la Recherche Scientifique, Belgium
Werner Schmutz
Affiliation:
ETH, Zürich, Switzerland
Ian R. Stevens
Affiliation:
School of Physics & Astronomy, Birmingham, United Kingdom

Extract

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Although substantial progress has been achieved since the discovery of X-ray emission from early-type stars with the EINSTEIN satellite, several crucial aspects of this phenomenon are still not fully understood. Considerable breakthroughs in this field are expected from observations with the X-ray Multi-Mirror satellite (XMM) due for launch in early 2000. XMM is the second cornerstone mission of the ESA Horizon 2000 science programme (see Lumb et al. 1996 and references therein for an overall description of the satellite). XMM offers a large effective area over a wide range of energies and its instrumentation provides simultaneously non-dispersive spectroscopic imaging (EPIC - European Photon Imaging Camera), medium-resolution dispersive spectroscopy (RGS - Reflection Grating Spectrometer) and optical-UV imaging (OM - Optical Monitor).

Type
Part 1. Basic observational properties of Wolf-Rayet stars and other hot massive stars
Information
Symposium - International Astronomical Union , Volume 193: Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies , 1999 , pp. 90 - 91
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

Corcoran, M.F. 1996, in: Niemela, V.S. & Morrell, N. (eds.), Collinding Winds in Binary Stars, RevMexAA-SC 5, 54 Google Scholar
Kaastra, J.S., Mewe, R., Nieuwenhuijzen, H. 1996, in: Yamashita, K. & Watanabe, T. (eds.), UV and X-ray Spectroscopy of Astrophysical and Laboratory Plasmas, (Tokyo: Univ. Acad. Press. Inc.), p. 411 Google Scholar
Lumb, D.H., Eggel, H., Lainé, R., Peacock, A.J. 1996, in: Siegmund, O.H. & Gummin, M.A. (eds.), EUV, X-ray, and Gamma Ray Instrumentation for Astronomy VII, Proc. SPIE, Vol. 2808, p. 326 Google Scholar
Pittard, J.M., Stevens, I.R. 1997, MNRAS 292, 298 Google Scholar