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Article: Cooling and spin-down of pulsars with evolving rotating equilibrium configuration. II. Effects of equations of state

TitleCooling and spin-down of pulsars with evolving rotating equilibrium configuration. II. Effects of equations of state
Authors
KeywordsEquation Of State
Nuclear Reactions, Nucleosynthesis, Abundances
Pulsars: General
Stars: Interiors
Stars: Rotation
Issue Date1993
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 1993, v. 417 n. 1, p. 279-286 How to Cite?
AbstractWe assume that an evolving rotating pulsar can be approximated by an equilibrium configuration of Maclaurin spheroid whose gravitational and rotational energies can be uniquely specified by stellar angular velocity Ω. Two heating mechanisms, namely the vortex creeping process and the crust-cracking process, are included in the evolution model. Various equations of state are used to construct stellar models, and therefore effects of stellar model on the cooling and spin-down of pulsars in such evolving rotating equilibrium configuration can be found. We show that the physical quantities of a pulsar, such as stellar radius, mass of crust region, surface gravity, density, and strength of crust, which are sensitive to the equation of state chosen for given mass and surface magnetic field, significantly affect the cooling and spin-down of pulsars with heating mechanisms. Exotic cooling processes, such as direct Urca neutrino emission process and pion condensation neutrino emission, are included in our calculation for specified stellar model. The heating mechanisms - the crust cracking and vortex creeping processes - are appreciably stronger in the stiffer star than in the softer one. In this paper, the observed data of pulsars, PSR 0531+21, PSR 0833-45, PSR 0656+14, PSR 1055-52, PSR 1929+10, and Geminga, are employed to put constraints on the heating parameters. Our results indicate that these constraints favors the pulsars to have stiff equation of state than soft one if heating mechanisms do exist.
Persistent Identifierhttp://hdl.handle.net/10722/174918
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369

 

DC FieldValueLanguage
dc.contributor.authorChong, Nen_US
dc.contributor.authorCheng, KSen_US
dc.date.accessioned2012-11-26T08:48:07Z-
dc.date.available2012-11-26T08:48:07Z-
dc.date.issued1993en_US
dc.identifier.citationAstrophysical Journal Letters, 1993, v. 417 n. 1, p. 279-286en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/174918-
dc.description.abstractWe assume that an evolving rotating pulsar can be approximated by an equilibrium configuration of Maclaurin spheroid whose gravitational and rotational energies can be uniquely specified by stellar angular velocity Ω. Two heating mechanisms, namely the vortex creeping process and the crust-cracking process, are included in the evolution model. Various equations of state are used to construct stellar models, and therefore effects of stellar model on the cooling and spin-down of pulsars in such evolving rotating equilibrium configuration can be found. We show that the physical quantities of a pulsar, such as stellar radius, mass of crust region, surface gravity, density, and strength of crust, which are sensitive to the equation of state chosen for given mass and surface magnetic field, significantly affect the cooling and spin-down of pulsars with heating mechanisms. Exotic cooling processes, such as direct Urca neutrino emission process and pion condensation neutrino emission, are included in our calculation for specified stellar model. The heating mechanisms - the crust cracking and vortex creeping processes - are appreciably stronger in the stiffer star than in the softer one. In this paper, the observed data of pulsars, PSR 0531+21, PSR 0833-45, PSR 0656+14, PSR 1055-52, PSR 1929+10, and Geminga, are employed to put constraints on the heating parameters. Our results indicate that these constraints favors the pulsars to have stiff equation of state than soft one if heating mechanisms do exist.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectEquation Of Stateen_US
dc.subjectNuclear Reactions, Nucleosynthesis, Abundancesen_US
dc.subjectPulsars: Generalen_US
dc.subjectStars: Interiorsen_US
dc.subjectStars: Rotationen_US
dc.titleCooling and spin-down of pulsars with evolving rotating equilibrium configuration. II. Effects of equations of stateen_US
dc.typeArticleen_US
dc.identifier.emailCheng, KS: hrspksc@hkucc.hku.hken_US
dc.identifier.authorityCheng, KS=rp00675en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.scopuseid_2-s2.0-12044258615en_US
dc.identifier.volume417en_US
dc.identifier.issue1en_US
dc.identifier.spage279en_US
dc.identifier.epage286en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridChong, N=43960969800en_US
dc.identifier.scopusauthoridCheng, KS=9745798500en_US

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