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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3163
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dc.contributor.authorDatta, B-
dc.contributor.authorHasan, S. S-
dc.contributor.authorSahu, P. K-
dc.contributor.authorPrasanna, A. R-
dc.date.accessioned2008-08-18T07:09:09Z-
dc.date.available2008-08-18T07:09:09Z-
dc.date.issued1998-02-
dc.identifier.citationInternational Journal of Modern Physics D, Vol. 7, No. 1, p. 49 - 59en
dc.identifier.issn0218-2718-
dc.identifier.urihttp://hdl.handle.net/2248/3163-
dc.description.abstractEigenfrequencies of radial pulsations of "slowly" rotating neutron stars are calculated in a general relativistic formalism given by Chandrasekhar and Friedman (1972). 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.extent3894 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherWorld Scientific Publishing Companyen
dc.relation.urihttp://en.scientificcommons.org/26055721en
dc.relation.urihttp://dx.doi.org/10.1142/S021827189800005Xen
dc.subjectNeutron Stars: Pulsationsen
dc.titleRadial modes of rotating neutron stars in the Chandrasekhar-Friedman formalismen
dc.typeArticleen
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