Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/3364
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dc.contributor.authorDatta, Bhaskar-
dc.contributor.authorThampan, Arun V.-
dc.contributor.authorBombaci, Ignazio-
dc.date.accessioned2008-01-03T09:25:16Z-
dc.date.available2008-01-03T09:25:16Z-
dc.date.issued1998-06-
dc.identifier.citationAstronomy and Astrophysics, 1998, Vol.334, p943-952en
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/2289/3364-
dc.descriptionOpen Accessen
dc.description.abstractFor four newly suggested realistic Equations of State of neutron star matter, we construct equilibrium sequences of rapidly rotating neutron stars in general relativity. The sequences are the normal and supramassive evolutionary sequences of constant rest mass. We find that for these equations of state the maximum (gravitational) mass rotating models occur (in central density and rotation rate Omega ) before the maximum-Omega models. We calculate equilibrium sequences for a constant value of Omega corresponding to the most rapidly rotating pulsar PSR 1937+21. Also calculated is the radius of the marginally stable orbit and its dependence on Omega , relevant for modeling of kilo-Hertz quasi-periodic oscillations in X-ray binaries.en
dc.format.extent331763 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherEuropean Southern Observatoryen
dc.relation.urihttp://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=1998A&A...334..943Den
dc.relation.urihttp://arxiv.org/abs/astro-ph/9801312en
dc.rights1998 European Southern Observatoryen
dc.subjectEQUATION OF STATE, PULSARSen
dc.subjectGENERAL RELATIVITYen
dc.subjectNEUTRON, STARS: ROTATIONen
dc.titleEquilibrium sequences of rotating neutron stars for new realistic Equations of Stateen
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

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