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Article: Cooling properties of Cloudy Bag strange stars

TitleCooling properties of Cloudy Bag strange stars
Authors
Issue Date2003
PublisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/astropartphys
Citation
Astroparticle Physics, 2003, v. 19 n. 1, p. 171-192 How to Cite?
AbstractAs the chiral symmetry is widely recognized as an important driver of the strong interaction dynamics, current strange stars models based on MIT bag models do not obey such symmetry. We investigate properties of bare strange stars using the Cloudy Bag model, in which a pion cloud coupled to the quark-confining bag is introduced such that chiral symmetry is conserved. The parameters in the model, namely the bag constant and strange quark mass are determined self-consistently by fitting the mass spectrum of baryons. Then the equation of state is obtained by evaluating the energy-momentum tensor of the system. We find that the stellar properties of the Cloudy Bag strange stars are similar to those of MIT Bag models. However, the decay of pions is a very efficient cooling way. In fact it can carry out most the thermal energy in a few milliseconds and directly convert them into 100 MeV photons via pion decay. This may be a very efficient c-ray burst mechanism. Numerical results indicate that temperature of a Cloudy Bag strange star is sufficiently lower than a MIT one for the small gap energy of color superconductivity (Δ = 1 MeV). On the other hand, large gap energy (Δ = 100 MeV) can suppress the pion emissivity and hence the cooling curves of Cloudy model and MIT model are almost identical. The long term cooling behaviors of both MIT model and Cloudy model are determined by the color-flavor locked phase. The surface luminosity of a bare strange star is higher than that of a neutron star until 106 and 108 s for (Δ = 100 MeV) and (Δ = 1 MeV) respectively. After this period, the surface luminosity of a bare strange star becomes lower than that of a neutron star even rapidly cooling mechanisms, e.g. direct URCA process or pion condensation, exist in the neutron stars. Hence, the cooling behavior may provide a possible way to distinguish a compact object between a neutron star, MIT strange star and Cloudy Bag strange star in observations. © 2002 Elsevier Science B.V. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/80711
ISSN
2015 Impact Factor: 3.425
2015 SCImago Journal Rankings: 1.612
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorNg, CYen_HK
dc.contributor.authorCheng, KSen_HK
dc.contributor.authorChu, MCen_HK
dc.date.accessioned2010-09-06T08:09:27Z-
dc.date.available2010-09-06T08:09:27Z-
dc.date.issued2003en_HK
dc.identifier.citationAstroparticle Physics, 2003, v. 19 n. 1, p. 171-192en_HK
dc.identifier.issn0927-6505en_HK
dc.identifier.urihttp://hdl.handle.net/10722/80711-
dc.description.abstractAs the chiral symmetry is widely recognized as an important driver of the strong interaction dynamics, current strange stars models based on MIT bag models do not obey such symmetry. We investigate properties of bare strange stars using the Cloudy Bag model, in which a pion cloud coupled to the quark-confining bag is introduced such that chiral symmetry is conserved. The parameters in the model, namely the bag constant and strange quark mass are determined self-consistently by fitting the mass spectrum of baryons. Then the equation of state is obtained by evaluating the energy-momentum tensor of the system. We find that the stellar properties of the Cloudy Bag strange stars are similar to those of MIT Bag models. However, the decay of pions is a very efficient cooling way. In fact it can carry out most the thermal energy in a few milliseconds and directly convert them into 100 MeV photons via pion decay. This may be a very efficient c-ray burst mechanism. Numerical results indicate that temperature of a Cloudy Bag strange star is sufficiently lower than a MIT one for the small gap energy of color superconductivity (Δ = 1 MeV). On the other hand, large gap energy (Δ = 100 MeV) can suppress the pion emissivity and hence the cooling curves of Cloudy model and MIT model are almost identical. The long term cooling behaviors of both MIT model and Cloudy model are determined by the color-flavor locked phase. The surface luminosity of a bare strange star is higher than that of a neutron star until 106 and 108 s for (Δ = 100 MeV) and (Δ = 1 MeV) respectively. After this period, the surface luminosity of a bare strange star becomes lower than that of a neutron star even rapidly cooling mechanisms, e.g. direct URCA process or pion condensation, exist in the neutron stars. Hence, the cooling behavior may provide a possible way to distinguish a compact object between a neutron star, MIT strange star and Cloudy Bag strange star in observations. © 2002 Elsevier Science B.V. All rights reserved.en_HK
dc.languageengen_HK
dc.publisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/astropartphysen_HK
dc.relation.ispartofAstroparticle Physicsen_HK
dc.rightsAstroparticle Physics. Copyright © Elsevier BV.en_HK
dc.titleCooling properties of Cloudy Bag strange starsen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0927-6505&volume=19&spage=171&epage=192&date=2003&atitle=Cooling+properties+of+Cloudy+Bag+strange+starsen_HK
dc.identifier.emailNg, CY: stephen_ng@hku.hken_HK
dc.identifier.emailCheng, KS: physhead@hku.hken_HK
dc.identifier.authorityNg, CY=rp01706en_HK
dc.identifier.authorityCheng, KS=rp00675en_HK
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1016/S0927-6505(02)00197-4en_HK
dc.identifier.scopuseid_2-s2.0-0037375239en_HK
dc.identifier.hkuros75851en_HK
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0037375239&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume19en_HK
dc.identifier.issue1en_HK
dc.identifier.spage171en_HK
dc.identifier.epage192en_HK
dc.identifier.isiWOS:000181705100012-
dc.publisher.placeNetherlandsen_HK
dc.identifier.scopusauthoridNg, CY=24830903500en_HK
dc.identifier.scopusauthoridCheng, KS=9745798500en_HK
dc.identifier.scopusauthoridChu, MC=7402457207en_HK

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