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Article: Properties of neutron stars in the relativistic mean-field theory

TitleProperties of neutron stars in the relativistic mean-field theory
Authors
KeywordsDense matter
Pulsars: General
Relativity
Stars: Interiors -
Stars: Neutron
Issue Date1996
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 1996, v. 464 n. 1 PART I, p. 348-353 How to Cite?
AbstractWe study the properties of dense matter in neutron stars and calculate the structure of the stars based on the Zimanyi & Moszkowski (ZM) model in the relativistic mean-field theory. We also compare these results with those based on the Boguta (BB) model with a recent satisfactory parameter set. The two models satisfy the requirements from the observations of the masses of binary radio pulsars, the rotation frequencies of millisecond pulsars, the redshifts of the e + annihilation lines of some y-ray bursts if they are neutron stars, and the crustal moment of inertia of neutron stars deduced from the glitch events. Other observations may provide a way to discriminate between the two models. We suggest that the most important observational discriminant between these two models is found by observing the surface radiation of neutron stars, since the BB model leads to a large photon fraction of neutron star matter and rapid cooling of neutron stars, but the ZM model does not. © 1996. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/43169
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorCheng, KSen_HK
dc.contributor.authorDai, ZGen_HK
dc.contributor.authorYao, CCen_HK
dc.date.accessioned2007-03-23T04:40:34Z-
dc.date.available2007-03-23T04:40:34Z-
dc.date.issued1996en_HK
dc.identifier.citationAstrophysical Journal Letters, 1996, v. 464 n. 1 PART I, p. 348-353en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/43169-
dc.description.abstractWe study the properties of dense matter in neutron stars and calculate the structure of the stars based on the Zimanyi & Moszkowski (ZM) model in the relativistic mean-field theory. We also compare these results with those based on the Boguta (BB) model with a recent satisfactory parameter set. The two models satisfy the requirements from the observations of the masses of binary radio pulsars, the rotation frequencies of millisecond pulsars, the redshifts of the e + annihilation lines of some y-ray bursts if they are neutron stars, and the crustal moment of inertia of neutron stars deduced from the glitch events. Other observations may provide a way to discriminate between the two models. We suggest that the most important observational discriminant between these two models is found by observing the surface radiation of neutron stars, since the BB model leads to a large photon fraction of neutron star matter and rapid cooling of neutron stars, but the ZM model does not. © 1996. The American Astronomical Society. All rights reserved.en_HK
dc.format.extent1141944 bytes-
dc.format.extent12158 bytes-
dc.format.mimetypeapplication/pdf-
dc.format.mimetypetext/plain-
dc.languageengen_HK
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_HK
dc.relation.ispartofAstrophysical Journal Lettersen_HK
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.rightsThe Astrophysical Journal. Copyright © University of Chicago Press.en_HK
dc.subjectDense matteren_HK
dc.subjectPulsars: Generalen_HK
dc.subjectRelativityen_HK
dc.subjectStars: Interiors -en_HK
dc.subjectStars: Neutronen_HK
dc.titleProperties of neutron stars in the relativistic mean-field theoryen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=464&spage=348&epage=353&date=1996&atitle=Properties+of+Neutron+Stars+in+the+Relativistic+Mean-Field+Theoryen_HK
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturepublished_or_final_versionen_HK
dc.identifier.doi10.1086/177325en_HK
dc.identifier.scopuseid_2-s2.0-21344448761en_HK
dc.identifier.hkuros20157-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-21344448761&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume464en_HK
dc.identifier.issue1 PART Ien_HK
dc.identifier.spage348en_HK
dc.identifier.epage353en_HK
dc.identifier.isiWOS:A1996UN84000032-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.scopusauthoridDai, ZG=7201387760en_HK
dc.identifier.scopusauthoridYao, CC=7201495781en_HK

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