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Article: Chemical heating in strange stars

TitleChemical heating in strange stars
Authors
KeywordsDense matter
Elementary particles
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. 468 n. 2 PART I, p. 819-822 How to Cite?
AbstractAs a strange star spins down, its core density increases, changing the chemical equilibrium state of strange matter. The relaxation toward the new equilibrium state takes a finite time, so the matter is not quite in chemical equilibrium, and energy is released by reactions at the expense of the stored chemical energy. We study such a chemical heating process for a spin-down strange star and find that this effect is significant at later times for weak magnetic fields. We compare the cooling of a strange star with that of an ordinary neutron star and find that the surface temperature of the strange star is much lower than that of the neutron star at the age up to 10 8 yr. This favorable to an observational signature for strange stars. © 1996. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/43181
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.date.accessioned2007-03-23T04:40:50Z-
dc.date.available2007-03-23T04:40:50Z-
dc.date.issued1996en_HK
dc.identifier.citationAstrophysical Journal Letters, 1996, v. 468 n. 2 PART I, p. 819-822en_HK
dc.identifier.issn2041-8205en_HK
dc.identifier.urihttp://hdl.handle.net/10722/43181-
dc.description.abstractAs a strange star spins down, its core density increases, changing the chemical equilibrium state of strange matter. The relaxation toward the new equilibrium state takes a finite time, so the matter is not quite in chemical equilibrium, and energy is released by reactions at the expense of the stored chemical energy. We study such a chemical heating process for a spin-down strange star and find that this effect is significant at later times for weak magnetic fields. We compare the cooling of a strange star with that of an ordinary neutron star and find that the surface temperature of the strange star is much lower than that of the neutron star at the age up to 10 8 yr. This favorable to an observational signature for strange stars. © 1996. The American Astronomical Society. All rights reserved.en_HK
dc.format.extent655603 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.subjectElementary particlesen_HK
dc.subjectStars: interiorsen_HK
dc.subjectStars: neutronen_HK
dc.titleChemical heating in strange starsen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-637X&volume=468&spage=819&epage=822&date=1996&atitle=Chemical+Heating+in+Strange+Starsen_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.doi10.1086/177737en_HK
dc.identifier.scopuseid_2-s2.0-21344459182en_HK
dc.identifier.hkuros21118-
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-21344459182&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume468en_HK
dc.identifier.issue2 PART Ien_HK
dc.identifier.spage819en_HK
dc.identifier.epage822en_HK
dc.identifier.isiWOS:A1996VE59600032-
dc.publisher.placeUnited Kingdomen_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.scopusauthoridDai, ZG=7201387760en_HK

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