Radial modes of rotating neutron stars in the Chandrasekhar-Friedman formalism

Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/3409

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DC Field	Value	Language
dc.contributor.author	Datta, Bhaskar	-
dc.contributor.author	Hasan, S.S.	-
dc.contributor.author	Sahu, P.K.	-
dc.contributor.author	Prasanna, A.R.	-
dc.date.accessioned	2008-02-01T11:07:41Z	-
dc.date.available	2008-02-01T11:07:41Z	-
dc.date.issued	1998-02	-
dc.identifier.citation	International Journal of Modern Physics D, 1998, Vol.7, p49-59	en
dc.identifier.issn	0218-2718	-
dc.identifier.uri	http://hdl.handle.net/2289/3409	-
dc.description	Restricted Access.	en
dc.description.abstract	Eigenfrequencies of radial pulsations of "slowly" rotating neutron stars are calculated in a general relativistic formalism given by Chandrasekhar & Friedman. It is found that the square of the frequencies are always a decreasing function of the central density of the neutron star. The decrease of the squared frequency is sensitive to the equation of state of neutron star matter, and is illustrated using realistic models.	en
dc.format.extent	762341 bytes	-
dc.format.mimetype	application/pdf	-
dc.language.iso	en	en
dc.publisher	World Scientific Publishing Company	en
dc.relation.uri	http://dx.doi.org/10.1142/S021827189800005X	en
dc.rights	1998. World Scientific Publishing Company	en
dc.title	Radial modes of rotating neutron stars in the Chandrasekhar-Friedman formalism	en
dc.type	Article	en
Appears in Collections:	Research Papers (A&A)

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