HEAD Division Meeting 1999, April 1999
Session 30. Other
Poster, Wednesday, April 14, 1999, 8:30am Wed. - 2:00pm Thurs., Gold Room

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[30.01] The X-ray ``MEGA'' Observing Campaign

Michael F. Corcoran (GSFC/LHEA/USRA)

The \textit{Einstein}, \textit{ROSAT} and \textit{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 \gamma2 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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