Thermal luminosity degeneracy of magnetized neutron stars with and without hyperon cores
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Título: | Thermal luminosity degeneracy of magnetized neutron stars with and without hyperon cores |
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Autor/es: | Anzuini, Filippo | Melatos, Andrew | Dehman, Clara | Viganò, Daniele | Pons, José A. |
Grupo/s de investigación o GITE: | Astrofísica Relativista |
Centro, Departamento o Servicio: | Universidad de Alicante. Departamento de Física Aplicada |
Palabras clave: | Stars: neutron | Stars: interiors | Stars: magnetic fields | Stars: evolution |
Área/s de conocimiento: | Astronomía y Astrofísica |
Fecha de publicación: | 17-may-2022 |
Editor: | Oxford University Press |
Cita bibliográfica: | Monthly Notices of the Royal Astronomical Society. 2022, 515(2): 3014-3027. https://doi.org/10.1093/mnras/stac1353 |
Resumen: | The dissipation of intense crustal electric currents produces high Joule heating rates in cooling neutron stars. Here it is shown that Joule heating can counterbalance fast cooling, making it difficult to infer the presence of hyperons (which accelerate cooling) from measurements of the observed thermal luminosity Lγ. Models with and without hyperon cores match Lγ of young magnetars (with poloidal-dipolar field Bdip ≳ 1014 G at the polar surface and Lγ ≳ 1034 erg s−1 at t ≲ 105 yr) as well as mature, moderately magnetized stars (with Bdip ≲ 1014 G and 1031 erg s−1 ≲ Lγ ≲ 1032 erg s−1 at t ≳ 105 yr). In magnetars, the crustal temperature is almost independent of hyperon direct Urca cooling in the core, regardless of whether the latter is suppressed or not by hyperon superfluidity. The thermal luminosities of light magnetars without hyperons and heavy magnetars with hyperons have Lγ in the same range and are almost indistinguishable. Likewise, Lγ data of neutron stars with Bdip ≲ 1014 G but with strong internal fields are not suitable to extract information about the equation of state as long as hyperons are superfluid, with maximum amplitude of the energy gaps of the order ≈1 MeV. |
Patrocinador/es: | FA is supported by The University of Melbourne through a Melbourne Research Scholarship. AM acknowledges funding from an Australian Research Council Discovery Project grant (DP170103625) and the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav) (CE170100004). DV is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (ERC Starting Grant "IMAGINE" No. 948582, PI DV). CD is supported by the ERC Consolidator Grant “MAGNESIA” (No. 817661, PI Nanda Rea) and this work has been carried out within the framework of the doctoral program in Physics of the Universitat Autònoma de Barcelona. JAP acknowledges support by the Generalitat Valenciana (PROMETEO/2019/071), AEI grant PGC2018-095984-B-I00 and the Alexander von Humboldt Stiftung through a Humboldt Research Award. |
URI: | http://hdl.handle.net/10045/123711 |
ISSN: | 0035-8711 (Print) | 1365-2966 (Online) |
DOI: | 10.1093/mnras/stac1353 |
Idioma: | eng |
Tipo: | info:eu-repo/semantics/article |
Derechos: | © 2022 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society |
Revisión científica: | si |
Versión del editor: | https://doi.org/10.1093/mnras/stac1353 |
Aparece en las colecciones: | INV - Astrofísica Relativista - Artículos de Revistas Investigaciones financiadas por la UE |
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Anzuini_etal_2022_MNRAS.pdf | 51,48 MB | Adobe PDF | Abrir Vista previa | |
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