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Article: Phase transitions in rotating neutron stars: Effects of stellar crusts

TitlePhase transitions in rotating neutron stars: Effects of stellar crusts
Authors
KeywordsDense matter
Stars: evolution
Stars: interiors
Stars: neutron
Stars: rotation
Issue Date2002
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2002, v. 564 n. 2 I, p. 909-913 How to Cite?
AbstractAs a rapidly rotating neutron star spins down due to the loss of its angular momentum, its central density increases and the nuclear matter in its core converts to quark matter, which leads to a drastic decrease of the stellar moment of inertia, and even results in an era of spin-up of the pulsar (Glendenning, Pei, & Weber 1997). We find that given a certain equation of state in the liquid core, even if the backbending of the moment of inertia as a function of the rotating frequency occurs, an increase of the total moment of inertia by only 1% could carry adequate angular momentum and stop the star spin-up. This small discrepancy in the total moment of inertia might be due to the different properties of subnuclear matter in the crust, especially to different transition density and pressure at the inner boundary of the solid crust between various models. The strong dependence of the phenomenon of back-bending on the physical state of the crust provides, in principle, a new observational approach to check and constrain theories on subnuclear matter.
Persistent Identifierhttp://hdl.handle.net/10722/43355
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.authorYuan, YFen_HK
dc.contributor.authorZhang, JLen_HK
dc.date.accessioned2007-03-23T04:44:10Z-
dc.date.available2007-03-23T04:44:10Z-
dc.date.issued2002en_HK
dc.identifier.citationAstrophysical Journal Letters, 2002, v. 564 n. 2 I, p. 909-913en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/43355-
dc.description.abstractAs a rapidly rotating neutron star spins down due to the loss of its angular momentum, its central density increases and the nuclear matter in its core converts to quark matter, which leads to a drastic decrease of the stellar moment of inertia, and even results in an era of spin-up of the pulsar (Glendenning, Pei, & Weber 1997). We find that given a certain equation of state in the liquid core, even if the backbending of the moment of inertia as a function of the rotating frequency occurs, an increase of the total moment of inertia by only 1% could carry adequate angular momentum and stop the star spin-up. This small discrepancy in the total moment of inertia might be due to the different properties of subnuclear matter in the crust, especially to different transition density and pressure at the inner boundary of the solid crust between various models. The strong dependence of the phenomenon of back-bending on the physical state of the crust provides, in principle, a new observational approach to check and constrain theories on subnuclear matter.en_HK
dc.format.extent114180 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.subjectStars: evolutionen_HK
dc.subjectStars: interiorsen_HK
dc.subjectStars: neutronen_HK
dc.subjectStars: rotationen_HK
dc.titlePhase transitions in rotating neutron stars: Effects of stellar crustsen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=564&issue=pt 1&spage=909&epage=913&date=2002&atitle=Phase+Transitions+in+Rotating+Neutron+Stars:+Effects+of+Stellar+Crustsen_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.doi10.1086/324330en_HK
dc.identifier.scopuseid_2-s2.0-0011592937en_HK
dc.identifier.hkuros68898-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0011592937&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume564en_HK
dc.identifier.issue2 Ien_HK
dc.identifier.spage909en_HK
dc.identifier.epage913en_HK
dc.identifier.isiWOS:000173166900034-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.scopusauthoridYuan, YF=35185850600en_HK
dc.identifier.scopusauthoridZhang, JL=15743325000en_HK

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