Effects of neutrino emissivity on the cooling of neutron stars in the presence of a strong magnetic field
One of the most interesting kind of neutron stars are the pulsars, which are highly magnetized neutron stars with fields up to 1014 G at the surface. The strength of magnetic field in the center of a neutron star remains unknown. According to the scalar virial theorem, magnetic field in the core cou...
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| description | One of the most interesting kind of neutron stars are the pulsars, which are highly magnetized neutron stars with fields up to 1014 G at the surface. The strength of magnetic field in the center of a neutron star remains unknown. According to the scalar virial theorem, magnetic field in the core could be as large as 1018 G. In this work we study the influence of strong magnetic fields on the cooling of neutron stars coming from direct Urca process. Direct Urca process is an extremely efficient mechanism for cooling a neutron star after its formation. The matter is described using a relativistic mean-field model at zero temperature with eight baryons (baryon octet), electrons and muons. We obtain the relative population of each species of particles as function of baryon density for different magnetic fields. We calculate numerically the cooling of neutron stars for a parametrized magnetic field and compare the results for the case without a magnetic field. |
| doi_str_mv | 10.1063/1.4937188 |
| format | Conference Proceeding |
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The strength of magnetic field in the center of a neutron star remains unknown. According to the scalar virial theorem, magnetic field in the core could be as large as 1018 G. In this work we study the influence of strong magnetic fields on the cooling of neutron stars coming from direct Urca process. Direct Urca process is an extremely efficient mechanism for cooling a neutron star after its formation. The matter is described using a relativistic mean-field model at zero temperature with eight baryons (baryon octet), electrons and muons. We obtain the relative population of each species of particles as function of baryon density for different magnetic fields. We calculate numerically the cooling of neutron stars for a parametrized magnetic field and compare the results for the case without a magnetic field.</description><identifier>ISSN: 0094-243X</identifier><identifier>EISSN: 1551-7616</identifier><identifier>DOI: 10.1063/1.4937188</identifier><language>eng</language><publisher>Melville: American Institute of Physics</publisher><subject>BARYON OCTETS ; BARYONS ; CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS ; COMPARATIVE EVALUATIONS ; COOLING ; Cooling effects ; DENSITY ; ELECTRONS ; EMISSIVITY ; MAGNETIC FIELDS ; Mathematical models ; MEAN-FIELD THEORY ; MUONS ; NEUTRINOS ; NEUTRON STARS ; Neutrons ; PARTICLES ; PULSARS ; RELATIVISTIC RANGE ; SCALARS ; Stars ; Stellar magnetic fields ; VIRIAL THEOREM</subject><ispartof>AIP conference proceedings, 2015, Vol.1693 (1)</ispartof><rights>2015 AIP Publishing LLC.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,309,310,314,776,780,785,786,881,23909,23910,25118,27901,27902</link.rule.ids><backlink>$$Uhttps://www.osti.gov/biblio/22494317$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Coelho, Eduardo Lenho</creatorcontrib><creatorcontrib>Chiapparini, Marcelo</creatorcontrib><creatorcontrib>Negreiros, Rodrigo Picanço</creatorcontrib><title>Effects of neutrino emissivity on the cooling of neutron stars in the presence of a strong magnetic field</title><title>AIP conference proceedings</title><description>One of the most interesting kind of neutron stars are the pulsars, which are highly magnetized neutron stars with fields up to 1014 G at the surface. The strength of magnetic field in the center of a neutron star remains unknown. According to the scalar virial theorem, magnetic field in the core could be as large as 1018 G. In this work we study the influence of strong magnetic fields on the cooling of neutron stars coming from direct Urca process. Direct Urca process is an extremely efficient mechanism for cooling a neutron star after its formation. The matter is described using a relativistic mean-field model at zero temperature with eight baryons (baryon octet), electrons and muons. We obtain the relative population of each species of particles as function of baryon density for different magnetic fields. We calculate numerically the cooling of neutron stars for a parametrized magnetic field and compare the results for the case without a magnetic field.</description><subject>BARYON OCTETS</subject><subject>BARYONS</subject><subject>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</subject><subject>COMPARATIVE EVALUATIONS</subject><subject>COOLING</subject><subject>Cooling effects</subject><subject>DENSITY</subject><subject>ELECTRONS</subject><subject>EMISSIVITY</subject><subject>MAGNETIC FIELDS</subject><subject>Mathematical models</subject><subject>MEAN-FIELD THEORY</subject><subject>MUONS</subject><subject>NEUTRINOS</subject><subject>NEUTRON STARS</subject><subject>Neutrons</subject><subject>PARTICLES</subject><subject>PULSARS</subject><subject>RELATIVISTIC RANGE</subject><subject>SCALARS</subject><subject>Stars</subject><subject>Stellar magnetic fields</subject><subject>VIRIAL THEOREM</subject><issn>0094-243X</issn><issn>1551-7616</issn><fulltext>true</fulltext><rsrctype>conference_proceeding</rsrctype><creationdate>2015</creationdate><recordtype>conference_proceeding</recordtype><recordid>eNpFj01LAzEYhIMoWKsH_0HA89Z8bZI9SqlWKHhR8LbsJu_bprRJ3aSC_96Vip4GZh6GGUJuOZtxpuU9n6lGGm7tGZnwuuaV0VyfkwljjaqEku-X5CrnLWOiMcZOSFgggiuZJqQRjmUIMVHYh5zDZyhfNEVaNkBdSrsQ13_UaOfSDZmGU34YIEN08AN0YzQCa7rv1hFKcBQD7Pw1ucBul-HmV6fk7XHxOl9Wq5en5_nDqkqC81IJL2WtXe8RO43MCw2SWWwENprVfS1Rou2t8r5HU1uvPArvLNcK-75DK6fk7tSbcgltdqGA27gU43izFUI1SnLzTx2G9HGEXNptOg5xHNYKLqTRijEmvwFkMmYS</recordid><startdate>20151217</startdate><enddate>20151217</enddate><creator>Coelho, Eduardo Lenho</creator><creator>Chiapparini, Marcelo</creator><creator>Negreiros, Rodrigo Picanço</creator><general>American Institute of Physics</general><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope></search><sort><creationdate>20151217</creationdate><title>Effects of neutrino emissivity on the cooling of neutron stars in the presence of a strong magnetic field</title><author>Coelho, Eduardo Lenho ; Chiapparini, Marcelo ; Negreiros, Rodrigo Picanço</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-o211t-2d3356cbdffa6f0d26e308f92f9605b53f3f8b84ddbf758d4df2dc8164fbbaf83</frbrgroupid><rsrctype>conference_proceedings</rsrctype><prefilter>conference_proceedings</prefilter><language>eng</language><creationdate>2015</creationdate><topic>BARYON OCTETS</topic><topic>BARYONS</topic><topic>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</topic><topic>COMPARATIVE EVALUATIONS</topic><topic>COOLING</topic><topic>Cooling effects</topic><topic>DENSITY</topic><topic>ELECTRONS</topic><topic>EMISSIVITY</topic><topic>MAGNETIC FIELDS</topic><topic>Mathematical models</topic><topic>MEAN-FIELD THEORY</topic><topic>MUONS</topic><topic>NEUTRINOS</topic><topic>NEUTRON STARS</topic><topic>Neutrons</topic><topic>PARTICLES</topic><topic>PULSARS</topic><topic>RELATIVISTIC RANGE</topic><topic>SCALARS</topic><topic>Stars</topic><topic>Stellar magnetic fields</topic><topic>VIRIAL THEOREM</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Coelho, Eduardo Lenho</creatorcontrib><creatorcontrib>Chiapparini, Marcelo</creatorcontrib><creatorcontrib>Negreiros, Rodrigo Picanço</creatorcontrib><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Coelho, Eduardo Lenho</au><au>Chiapparini, Marcelo</au><au>Negreiros, Rodrigo Picanço</au><format>book</format><genre>proceeding</genre><ristype>CONF</ristype><atitle>Effects of neutrino emissivity on the cooling of neutron stars in the presence of a strong magnetic field</atitle><btitle>AIP conference proceedings</btitle><date>2015-12-17</date><risdate>2015</risdate><volume>1693</volume><issue>1</issue><issn>0094-243X</issn><eissn>1551-7616</eissn><abstract>One of the most interesting kind of neutron stars are the pulsars, which are highly magnetized neutron stars with fields up to 1014 G at the surface. The strength of magnetic field in the center of a neutron star remains unknown. According to the scalar virial theorem, magnetic field in the core could be as large as 1018 G. In this work we study the influence of strong magnetic fields on the cooling of neutron stars coming from direct Urca process. Direct Urca process is an extremely efficient mechanism for cooling a neutron star after its formation. The matter is described using a relativistic mean-field model at zero temperature with eight baryons (baryon octet), electrons and muons. We obtain the relative population of each species of particles as function of baryon density for different magnetic fields. We calculate numerically the cooling of neutron stars for a parametrized magnetic field and compare the results for the case without a magnetic field.</abstract><cop>Melville</cop><pub>American Institute of Physics</pub><doi>10.1063/1.4937188</doi></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0094-243X |
| ispartof | AIP conference proceedings, 2015, Vol.1693 (1) |
| issn | 0094-243X 1551-7616 |
| language | eng |
| recordid | cdi_osti_scitechconnect_22494317 |
| source | AIP Journals Complete |
| subjects | BARYON OCTETS BARYONS CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS COMPARATIVE EVALUATIONS COOLING Cooling effects DENSITY ELECTRONS EMISSIVITY MAGNETIC FIELDS Mathematical models MEAN-FIELD THEORY MUONS NEUTRINOS NEUTRON STARS Neutrons PARTICLES PULSARS RELATIVISTIC RANGE SCALARS Stars Stellar magnetic fields VIRIAL THEOREM |
| title | Effects of neutrino emissivity on the cooling of neutron stars in the presence of a strong magnetic field |
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