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dc.contributor.authorMickaliger, M. B.
dc.contributor.authorHu, Chin-Ping
dc.contributor.authorLyne, A. G.
dc.contributor.authorShaw, B.
dc.contributor.authorSurnis, M. P.
dc.contributor.authorRajwade, K. M.
dc.contributor.authorStappers, B. W.
dc.contributor.authorLiu, K.
dc.contributor.authorKramer, M.
dc.contributor.authorDesvignes, G.
dc.contributor.authorKaruppusamy, R.
dc.contributor.authorEnoto, T.
dc.contributor.authorGuver, T.
dc.date.accessioned2022-07-04T13:28:31Z
dc.date.available2022-07-04T13:28:31Z
dc.date.issued2022
dc.identifier.citationRajwade K. M. , Stappers B. W. , Lyne A. G. , Shaw B., Mickaliger M. B. , Liu K., Kramer M., Desvignes G., Karuppusamy R., Enoto T., et al., "Long term radio and X-ray evolution of the magnetar Swift J1818.0-1607", MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, cilt.512, sa.2, ss.1687-1695, 2022
dc.identifier.issn0035-8711
dc.identifier.othervv_1032021
dc.identifier.otherav_4b038d15-1aee-482c-99f6-5f0f365d2527
dc.identifier.urihttp://hdl.handle.net/20.500.12627/182633
dc.identifier.urihttps://doi.org/10.1093/mnras/stac446
dc.identifier.urihttps://avesis.istanbul.edu.tr/api/publication/4b038d15-1aee-482c-99f6-5f0f365d2527/file
dc.description.abstractWe report on the the long term monitoring campaign of the seemingly youngest magnetar Swift J1818.0-1607 at radio and X-ray wavelengths over a span of one year. We obtained a coherent timing solution for the magnetar over the same time span. The frequency derivative of the magnetar shows systematic variation with the values oscillating about a mean value of -1.37 x 10(-11) Hz s(-1). The magnitude of the variation in the frequency derivative reduces with time before converging on the mean value. This corresponds to a characteristic age of similar to 860 years, 2-4 times more than previously estimated. We were able to identify four states in the spin-frequency derivative that were quantified by the amount of modulation about the mean value and the transition between these states seem to be correlated with the change in the radio emission of the magnetar while no correlation is seen in the average radio profile variability on a shorter time-scale (days). The 0.5-12 keV X-ray flux shows a monotonic decrease that can be attributed to thermal emission from a hot spot on the surface of the neutron star that is reducing in size. Such decrease is consistent with what is seen in other magnetars. The potential correlation between the radio emission mode and the behaviour of the spin-down rate hints to a global change in the magnetopshere of the magnetar akin to the correlation seen in a subset of mode-changing radio pulsars and suggests a physical link between the two sub-populations.
dc.language.isoeng
dc.subjectPhysical Sciences
dc.subjectFizik
dc.subjectASTRONOMİ VE ASTROFİZİK
dc.subjectUzay bilimi
dc.subjectTemel Bilimler (SCI)
dc.subjectAstronomi ve Astrofizik
dc.subjectTemel Bilimler
dc.subjectPhysics and Astronomy (miscellaneous)
dc.subjectGeneral Physics and Astronomy
dc.subjectSpace and Planetary Science
dc.subjectAstronomy and Astrophysics
dc.titleLong term radio and X-ray evolution of the magnetar Swift J1818.0-1607
dc.typeMakale
dc.relation.journalMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
dc.contributor.departmentUniversity of Manchester , ,
dc.identifier.volume512
dc.identifier.issue2
dc.identifier.startpage1687
dc.identifier.endpage1695
dc.contributor.firstauthorID3404114


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