Crust–magnetosphere coupling during magnetar evolution and implications for the surface temperature

Please use this identifier to cite or link to this item: http://hdl.handle.net/10045/82733
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dc.contributorAstrofísica Relativistaes_ES
dc.contributor.authorAkgün, Taner-
dc.contributor.authorCerdá-Durán, Pablo-
dc.contributor.authorMiralles, Juan A.-
dc.contributor.authorPons, José A.-
dc.contributor.otherUniversidad de Alicante. Departamento de Física Aplicadaes_ES
dc.date.accessioned2018-10-29T12:31:36Z-
dc.date.available2018-10-29T12:31:36Z-
dc.date.issued2018-12-21-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society. 2018, 481(4): 5331-5338. doi:10.1093/mnras/sty2669es_ES
dc.identifier.issn0035-8711 (Print)-
dc.identifier.issn1365-2966 (Online)-
dc.identifier.urihttp://hdl.handle.net/10045/82733-
dc.description.abstractWe study the coupling of the force-free magnetosphere to the long-term internal evolution of a magnetar. We allow the relation between the poloidal and toroidal stream functions – that characterizes the magnetosphere – to evolve freely without constraining its particular form. We find that, on time-scales of the order of kyr, the energy stored in the magnetosphere gradually increases, as the toroidal region grows and the field lines expand outwards. This continues until a critical point is reached beyond which force-free solutions for the magnetosphere can no longer be constructed, likely leading to some large-scale magnetospheric reorganization. The energy budget available for such events can be as high as several 1045 erg for fields of 1014 G. Subsequently, starting from the new initial conditions, the evolution proceeds in a similar manner. The time-scale to reach the critical point scales inversely with the magnetic field amplitude. Allowing currents to pass through the last few metres below the surface, where the magnetic diffusivity is orders of magnitude larger than in the crust, should give rise to a considerable amount of energy deposition through Joule heating. We estimate that the effective surface temperature could increase locally from ∼0.1 keV to ∼0.3-0.6 keV, in good agreement with observations. Similarly, the power input from the interior into the magnetosphere could be as high as 1035-1036 erg s−1, which is consistent with peak luminosities observed during magnetar outbursts. Therefore, a detailed treatment of currents flowing through the envelope may be needed to explain the thermal properties of magnetars.es_ES
dc.description.sponsorshipThis work is supported in part by the Spanish MINECO/FEDER grants AYA2015-66899-C2-1-P, AYA2015-66899-C2-2-P, the grant of Generalitat Valenciana PROMETEOII-2014-069, and by the PHAROS COST action CA16214. PC acknowledges the support from the Ramón y Cajal program of the Spanish MINECO (RYC-2015-19074).es_ES
dc.languageenges_ES
dc.publisherOxford University Presses_ES
dc.rights© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Societyes_ES
dc.subjectMagnetic fieldses_ES
dc.subjectMHDes_ES
dc.subjectStars: magnetarses_ES
dc.subjectStars: magnetic fieldes_ES
dc.subjectStars: neutrones_ES
dc.subject.otherAstronomía y Astrofísicaes_ES
dc.titleCrust–magnetosphere coupling during magnetar evolution and implications for the surface temperaturees_ES
dc.typeinfo:eu-repo/semantics/articlees_ES
dc.peerreviewedsies_ES
dc.identifier.doi10.1093/mnras/sty2669-
dc.relation.publisherversionhttps://doi.org/10.1093/mnras/sty2669es_ES
dc.rights.accessRightsinfo:eu-repo/semantics/openAccesses_ES
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