The X-ray ``MEGA'' Observing Campaign

Details The X-ray ``MEGA'' Observing Campaign The X-ray ``MEGA'' Observing Campaign

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999head....4.3001c&link_type=abstract

American Astronomical Society, HEAD meeting #4, #30.01; Bulletin of the American Astronomical Society, Vol. 31, p.733

Astronomy and Astrophysics

Astronomy

Scientific paper

The Einstein, ROSAT and ASCA X-ray observatories have made substantial progress towards an understanding of X-ray emission from massive stars, having established (for example) that the observed X-ray luminosity is proportional to stellar bolometric luminosity for the OB stars, or that X-ray variability is relatively rare among massive stars, or that X-ray emission from Wolf-Rayet stars shows unexpectedly large amounts of scatter in their Lx/Lbol relation, or that binary systems like WR 140 and gamma (2) Vel show evidence of X-ray emitting gas produced by the collision of stellar winds. These observations have also raised many unresolved questions: why are some binaries X-ray variables and some not? What causes the scatter in Lx/Lbol for the WR stars? Why are LBVs weak X-ray sources? When is X-ray emission from colliding winds important, and what does that tell us about the nature of the stellar winds in binaries? Modern X-ray observatories raise the exciting possibility of using X-ray emission as a tool to address fundamental questions about the dynamics and chemistry of stellar winds. The X-ray "MEGA" Campaign consists of 50 scientists with interest in developing a full understanding of the phenomena of X-ray emission from hot stars. The purpose of this campaign is to obtain deep X-ray observations of important massive stars and star clusters, along with supporting ground-based observations in order to fully understand the relation between stellar atmospheric phenomena and X-ray emission from hot massive stars. We discuss some recent observing campaigns and results of our observations.

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