Abstract

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⊙~

Publication Date

5-1-2002

Comments

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.

Document Type

Article

Department, Program, or Center

Chester F. Carlson Center for Imaging Science (COS)

Campus

RIT – Main Campus

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