X–RAY EMISSION OF THE PULSAR–Be STAR BINARY PSR 1259–63*
نویسنده
چکیده
X–rays are detected from the pulsar–Be star binary PSR 1259−63 only after apastron passage. We suggest that the X–rays result from accretion on to the pulsar magnetosphere of matter captured from the Be star wind. The capture efficiency changes markedly at this phase, in line with the observations, provided that the wind is slow (∼ sonic) at large distances from the Be star. Accepted by The Astrophysical Journal ∗Work supported in part by grant from the NASA ROSAT Guest Investigator Program, NAG 5–1684, and by Department of Energy contract DE–AC03–76SF00515 (SLAC). ¦Permanent Address: Sonoma State University. ?Visiting Professor, Stanford Linear Accelerator Center
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