Rotochemical heating in millisecond pulsars

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dc.contributor.authorFernández, R
dc.contributor.authorReisenegger, A
dc.date.accessioned2025-01-21T01:06:59Z
dc.date.available2025-01-21T01:06:59Z
dc.date.issued2005
dc.description.abstractRotochemical heating originates in a departure from beta equilibrium due to spin-down compression in a rotating neutron star. The main consequence is that the star eventually arrives at a quasi-equilibrium state in which the thermal photon luminosity depends only on the current value of the spin-down power, which is directly measurable. Only in millisecond pulsars does the spin-down power remain high long enough for this state to be reached with a substantial luminosity. We report an extensive study of the effect of this heating mechanism on the thermal evolution of millisecond pulsars, developing a general formalism in the slow-rotation approximation of general relativity that takes the spatial structure of the star fully into account, and using a sample of realistic equations of state to solve the nonsuperfluid case numerically. We show that nearly all observed millisecond pulsars are very likely to be in the quasi-equilibrium state. Our predicted quasi-equilibrium temperatures for PSR J0437-4715 are only 20% lower than inferred from observations. Accounting for superfluidity should increase the predicted value.
dc.fuente.origenWOS
dc.identifier.issn0004-637X
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/96256
dc.identifier.wosidWOS:000229046600027
dc.issue.numero1
dc.language.isoen
dc.pagina.final306
dc.pagina.inicio291
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.subjectdense matter
dc.subjectpulsars : general
dc.subjectpulsars : individual ( PSR J0108-1431, PSR J0437-4715)
dc.subjectrelativity
dc.subjectstars : neutron
dc.subjectstars : rotation
dc.titleRotochemical heating in millisecond pulsars
dc.typeartículo
dc.volumen625
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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