dc.contributor.author | Gogus, Ersin | |
dc.contributor.author | Guver, Tolga | |
dc.contributor.author | Ozel, Feryal | |
dc.date.accessioned | 2021-03-03T21:22:47Z | |
dc.date.available | 2021-03-03T21:22:47Z | |
dc.date.issued | 2015 | |
dc.identifier.citation | Guver T., Gogus E., Ozel F., "MAPPING THE SURFACE OF THE MAGNETAR 1E 1048.1-5937 IN OUTBURST AND QUIESCENCE THROUGH PHASE-RESOLVED X-RAY SPECTROSCOPY", ASTROPHYSICAL JOURNAL, cilt.801, sa.1, 2015 | |
dc.identifier.issn | 0004-637X | |
dc.identifier.other | av_5ed43553-3512-4b13-9cb2-e9ac74b01097 | |
dc.identifier.other | vv_1032021 | |
dc.identifier.uri | http://hdl.handle.net/20.500.12627/66282 | |
dc.identifier.uri | https://doi.org/10.1088/0004-637x/801/1/48 | |
dc.description.abstract | We model the pulse profiles and the phase-resolved spectra of the anomalous X-ray pulsar 1E 1048.1-5937 obtained with XMM-Newton to map its surface temperature distribution during an active and a quiescent epoch. We develop and apply a model that takes into account the relevant physical and geometrical effects on the neutron star surface, magnetosphere, and spacetime. Using this model, we determine the observables at infinity as a function of pulse phase for different numbers and sizes of hot spots on the surface. We show that the pulse profiles extracted from both observations can be modeled with a single hot spot and an antipodal cool component. The size of the hot spot changes from approximate to 80 degrees in 2007, three months after the onset of a dramatic flux increase, to approximate to 30 degrees during the quiescent observation in 2011, when the pulsed fraction returned to the pre-outburst approximate to 65% level. For the 2007 observation, we also find that a model consisting of a single 0.4 keV hot spot with a magnetic field strength of 1.8 x 10(14) G accounts for the spectra obtained at three different pulse phases but underpredicts the flux at the pulse minimum, where the contribution to the emission from the cooler component is non-negligible. The inferred temperature of the spot stays approximately constant between different pulse phases, in agreement with a uniform temperature, single hot spot model. These results suggest that the emitting area grows significantly during outbursts but returns to its persistent and significantly smaller size within a timescale of a few years. | |
dc.language.iso | eng | |
dc.subject | Uzay bilimi | |
dc.subject | Temel Bilimler | |
dc.subject | Astronomi ve Astrofizik | |
dc.subject | Fizik | |
dc.subject | Temel Bilimler (SCI) | |
dc.subject | ASTRONOMİ VE ASTROFİZİK | |
dc.title | MAPPING THE SURFACE OF THE MAGNETAR 1E 1048.1-5937 IN OUTBURST AND QUIESCENCE THROUGH PHASE-RESOLVED X-RAY SPECTROSCOPY | |
dc.type | Makale | |
dc.relation.journal | ASTROPHYSICAL JOURNAL | |
dc.contributor.department | Sabancı Üniversitesi , , | |
dc.identifier.volume | 801 | |
dc.identifier.issue | 1 | |
dc.contributor.firstauthorID | 87594 | |