Show simple item record

dc.contributor.authorDall'Osso, S.
dc.contributor.authorGranot, J.
dc.contributor.authorPiran, T.
dc.date.accessioned2012-08-08T14:00:24Z
dc.date.available2012-08-08T14:00:24Z
dc.date.issued2012-06
dc.identifier.citationDall'Osso , S , Granot , J & Piran , T 2012 , ' Magnetic field decay in neutron stars : from soft gamma repeaters to weak-field magnetars' ' , Monthly Notices of the Royal Astronomical Society , vol. 422 , no. 4 , pp. 2878-2903 . https://doi.org/10.1111/j.1365-2966.2012.20612.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 921467
dc.identifier.otherPURE UUID: 26f25f5b-729c-4beb-bfef-77c86d0672c8
dc.identifier.otherWOS: 000304246100009
dc.identifier.otherScopus: 84861231162
dc.identifier.urihttp://hdl.handle.net/2299/8821
dc.description.abstractThe recent discovery of the weak-field, old magnetar soft gamma repeater (SGR) J0418+5729, whose dipole magnetic field, Bdip, is less than 7.5 x 10(12) G, has raised perplexing questions: how can the neutron star produce SGR-like bursts with such a low magnetic field? What powers the observed X-ray emission when neither the rotational energy nor the magnetic dipole energy is sufficient? These observations, which suggest either a much larger energy reservoir or a much younger true age (or both), have renewed the interest in the evolutionary sequence of magnetars. We examine here a phenomenological model for the magnetic field decay: and compare its predictions with the observed period, P, the period derivative, , and the X-ray luminosity, LX, of magnetar candidates. We find a strong evidence for a dipole field decay on a time-scale of similar to 10(3) yr for the strongest (Bdip similar to 10(15) G) field objects, with a decay index within the range 1 =a < 2 and more likely within 1.5 less than or similar to alpha a less than or similar to 1.8. The decaying field implies a younger age than what is implied by . Surprisingly, even with the younger age, the energy released in the dipole field decay is insufficient to power the X-ray emission, suggesting the existence of a stronger internal field, Bint. Examining several models for the internal magnetic field decay, we find that it must have a very large (greater than or similar to 10(16) G) initial value. Our findings suggest two clear distinct evolutionary tracks the SGR/anomalous X-ray pulsar branch and the transient branch, with a possible third branch involving high-field radio pulsars that age into low-luminosity X-ray dim isolated neutron stars.en
dc.format.extent26
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights/dk/atira/pure/core/openaccesspermission/embargoed
dc.titleMagnetic field decay in neutron stars : from soft gamma repeaters to weak-field magnetars'en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.date.embargoedUntil2012-12-01
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Accepted Version
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2012.20612.x
rioxxterms.licenseref.startdate2012-12-01Z
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.date.embargo2012-12-01Z
herts.rights.accesstypeopenAccess


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record