Disk Luminosity for Accreting, Weak Magnetic Field Neutron Stars in the ``Slow'' Rotation Approximation

Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/4187

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DC Field	Value	Language
dc.contributor.author	Datta, B	-
dc.date.accessioned	2008-12-29T12:18:18Z	-
dc.date.available	2008-12-29T12:18:18Z	-
dc.date.issued	1999	-
dc.identifier.citation	Arzoumanian, Z., Van der Hooft, and van den Heuvel, E. P. J., eds., Pulsar Timing, General Relativity and the Internal Structure of Neutron Stars., Published by Koninklijke Nederlandse Akademie van Wetenschappen, Amsterdam, The Netherlands 1999, pp. 287.	en
dc.identifier.uri	http://hdl.handle.net/2248/4187	-
dc.description.abstract	For accretion onto neutron stars possessing weak surface magnetic fields and substantial rotation rates (corresponding to the secular instability limit), we calculate the disk and surface layer luminosities general relativistically using the Hartle & Thorne formalism, and illustrate these quantities for a set of representative neutron star equations of state.	en
dc.language.iso	en	en
dc.publisher	Koninklijke Nederlandse Akademie van Wetenschappen	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1999ptgr.conf..287D	en
dc.title	Disk Luminosity for Accreting, Weak Magnetic Field Neutron Stars in the ``Slow'' Rotation Approximation	en
dc.type	Article	en
Appears in Collections:	IIAP Publications

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