A highly resistive layer within the crust of X-ray pulsars limits their spin periods
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Campo DC | Valor | Idioma |
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dc.contributor | Astrofísica Relativista | es |
dc.contributor.author | Pons, José A. | - |
dc.contributor.author | Viganò, Daniele | - |
dc.contributor.author | Rea, Nanda | - |
dc.contributor.other | Universidad de Alicante. Departamento de Física Aplicada | es |
dc.date.accessioned | 2013-11-14T10:42:58Z | - |
dc.date.available | 2013-11-14T10:42:58Z | - |
dc.date.issued | 2013-06-09 | - |
dc.identifier.citation | Nature Physics. 2013, 9: 431-434. doi:10.1038/nphys2640 | es |
dc.identifier.issn | 1745-2473 (Print) | - |
dc.identifier.issn | 1745-2481 (Online) | - |
dc.identifier.uri | http://hdl.handle.net/10045/33858 | - |
dc.description.abstract | The lack of isolated X-ray pulsars with spin periods longer than 12 s raises the question of where the population of evolved high-magnetic-field neutron stars has gone. Unlike canonical radiopulsars, X-ray pulsars are not subject to physical limits to the emission mechanism nor observational biases against the detection of sources with longer periods. Here we show that a highly resistive layer in the innermost part of the crust of neutron stars naturally limits the spin period to a maximum value of about 10–20 s. This highly resistive layer is expected if the inner crust is amorphous and heterogeneous in nuclear charge, possibly owing to the existence of a nuclear ‘pasta’ phase. Our findings suggest that the maximum period of isolated X-ray pulsars may be the first observational evidence for an amorphous inner crust, whose properties can be further constrained by future X-ray timing missions combined with more detailed models. | es |
dc.description.sponsorship | This work has been supported by the Spanish MEC grants AYA 2010-21097-C03-02, AYA2012-39303, SGR2009-811, TW2010005 and iLINK 2011-0303. NR is supported by a Ramon y Cajal Research Fellowship and DV by the Prometeo/2009/103 grant. | es |
dc.language | eng | es |
dc.publisher | Nature Publishing Group | es |
dc.rights | © 2013 Nature Publishing Group | es |
dc.subject | X-ray pulsars | es |
dc.subject | Spin periods | es |
dc.subject | Highly resistive layer | es |
dc.subject | Crust of neutron stars | es |
dc.subject | Nuclear ‘pasta’ phase | es |
dc.subject.other | Astronomía y Astrofísica | es |
dc.title | A highly resistive layer within the crust of X-ray pulsars limits their spin periods | es |
dc.type | info:eu-repo/semantics/article | es |
dc.peerreviewed | si | es |
dc.identifier.doi | 10.1038/nphys2640 | - |
dc.relation.publisherversion | http://dx.doi.org/10.1038/nphys2640 | es |
dc.rights.accessRights | info:eu-repo/semantics/openAccess | es |
Aparece en las colecciones: | INV - Astrofísica Relativista - Artículos de Revistas |
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2013_Pons_Vigano_Rea_NaturePhys-pre.pdf | Preprint (acceso abierto) | 239,73 kB | Adobe PDF | Abrir Vista previa |
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