We study the conditions under which a main sequence binary companion to the central ionizing star of a planetary nebula (PN) might become magnetically active and thereby display strong X-ray luminosity, Lx~> 5×10^29 erg s^−1. Since most PNe are older than few billion years, any main sequence companion will rotate too slowly to have magnetic activity and hence bright X-ray emission, unless it is spun-up. We demonstrate that if the orbital separation during the AGB phase of the PN progenitor is a~<30 − 60 AU, main sequence companions in the spectral type range F7 to M4 (mass range 0.3M⊙~

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Also archived in: arXiv: astro-ph/0111266 v1 14 Nov 2001 We thank Rob Jeffries for helpful comments. N. S. was supported by a Celerity Foundation Distinguished Visiting Scholar grant at the University of Virginia. This research was supported in part by grants from the US-Israel Binational Science Foundation, and by NASA/Chandra X-ray Center (Smithsonian Astrophysical Observatory) grant GO 0-1067X to R. I. T.ISSN:1538-4365 Note: imported from RIT’s Digital Media Library running on DSpace to RIT Scholar Works in February 2014.

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Department, Program, or Center

Chester F. Carlson Center for Imaging Science (COS)


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