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Accretion onto magnetized neutron stars - X-ray pulsars with intermediate rotation ratesAssuming that the accreting material originates in a wind or envelope and therefore carried no net angular momentum, the Kevin-Helmholtz instability is applied to the transport of accreting plasma across the magnetopause of a rotating and magnetized neutron star for the case in which this surface is interchange-stable. Magnetopause location is determined, and the blackbody emission temperature is estimated. A possible period-dependence is noted in the X-ray temperature data which is in approximate agreement with the present model calculations. The magnetopause is found to be insufficiently stable to support an optically thick sheath of plasma surrounding the source, so that neither shrouding of the X-ray source nor significant reprocessing of the radiation field is possible in the model presented. It is concluded that while the flow structure at the magnetopause can control accretion column geometry, the emerging pulse profile and spectra are only indirectly altered, through a dynamical influence on emission region geometry.
Document ID
19830044497
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Burnard, D. J.
(California Univ. Berkeley, CA, United States)
Arons, J.
(California, University Berkeley, CA, United States)
Lea, S. M.
(California, University Berkeley, CA; San Francisco State University, San Francisco, CA, United States)
Date Acquired
August 11, 2013
Publication Date
March 1, 1983
Publication Information
Publication: Astrophysical Journal
Subject Category
Astrophysics
Accession Number
83A25715
Funding Number(s)
CONTRACT_GRANT: NAS8-33357
CONTRACT_GRANT: NSF AST-79-23243
CONTRACT_GRANT: NSF AST-78-21070
CONTRACT_GRANT: NAG8-385
Distribution Limits
Public
Copyright
Other

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