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Borghese, A; Rea, N; Turolla, R; Rigoselli, M; Alford, J A J; Gotthelf, E V; Burgay, M; Possenti, A; Zane, S; Coti Zelati, F; Perna, R; Esposito, P; Mereghetti, S; Viganò, D; Tiengo, A; Götz, D; Ibrahim, A; Israel, G L; Pons, J; Sathyaprakash, R
Monthly notices of the Royal Astronomical Society, 07/2021, Letnik: 504, Številka: 4Journal Article
ABSTRACT After 15 yr, in late 2018, the magnetar XTE J1810−197 underwent a second recorded X-ray outburst event and reactivated as a radio pulsar. We initiated an X-ray monitoring campaign to follow the timing and spectral evolution of the magnetar as its flux decays using Swift, XMM–Newton, NuSTAR, and NICER observations. During the year-long campaign, the magnetar reproduced similar behaviour to that found for the first outburst, with a factor of 2 change in its spin-down rate from ∼7.2 × 10−12 to ∼1.5 × 10−11 s s−1 after two months. Unique to this outburst, we confirm the peculiar energy-dependent phase shift of the pulse profile. Following the initial outburst, the spectrum of XTE J1810−197 is well modelled by multiple blackbody components corresponding to a pair of non-concentric, hot thermal caps surrounded by a cooler one, superposed to the colder star surface. We model the energy-dependent pulse profile to constrain the viewing and surface emission geometry and find that the overall geometry of XTE J1810−197 has likely evolved relative to that found for the 2003 event.
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