XMM-Newton reveals a candidate period for the spin of the “Magnificent Seven” neutron star RX J1605.3+3249
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In this article, the authors used phase-resolved spectroscopy with the XMM-Newton Observatory for 60 ks aiming at unveiling the neutron star rotation rate and investigating its spectrum in detail.Abstract:
Context. The group of seven thermally emitting isolated neutron stars (INSs) discovered by ROSAT and known as the “Magnificent Seven” (M7) is unique among the various neutron star populations. Crustal heating by means of magnetic field decay and an evolutionary link with magnetars may explain why these objects rotate more slowly and have higher thermal luminosities and magnetic field intensities than standard rotation-powered pulsars of similar age. Aims. The third brightest INS, RX J1605.3+3249, is the only object amidst the seven still lacking a detected periodicity. The source spectrum, while purely thermal with no significant magnetospheric emission, is complex and displays both narrow and broad absorption features that can potentially be used to constrain the surface component of the magnetic field, as well as the mass-to-radius ratio of the neutron star. Methods. We observed the source with the XMM-Newton Observatory for 60 ks aiming at unveiling the neutron star rotation rate and investigating its spectrum in detail. We confront our results with previous observations of the source and discuss its properties in the context of the M7 as a group and of the known population of Galactic INSs. Results. A periodic signal at P = 3.387864(16) s, most likely the neutron star spin period, is detected at the 4σ confidence level. The amplitude of the modulation was found to be energy dependent and is more significantly detected when the timing search is restricted to photons with energy higher than ∼0.5 keV. The coherent combination of the new data with a past XMM-Newton EPIC-pn observation of the source constrains the pulsar spin-down rate at the 2σ confidence level, u ν ∼− 1.39 × 10 −13 Hz s −1 , implying a dipolar magnetic field of Bdip ∼ 7.4 × 10 13 G. If confirmed, RX J1605.3+3249 would be the neutron star with the highest dipolar field amongst the M7. The spectrum of the source shows evidence of a cool blackbody component, as well as for the presence of two broad absorption features. Furthermore, high-resolution spectroscopy with the RGS cameras confirms the presence of a narrow absorption feature at energy ∼0.57 keV in the co-added spectrum of the source, also seen in other thermally emitting isolated neutron stars. Conclusions. Phase-resolved spectroscopy, as well as a dedicated observing campaign aimed at determining a timing solution, will give invaluable constraints on the neutron star geometry and will allow one to confirm the high value of spin down, which would place the source closer to a magnetar than any other M7 INS.read more
Citations
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Journal ArticleDOI
Cyclotron lines in highly magnetized neutron stars
Ruediger Staubert,Joachim Trümper,Eckhard Kendziorra,D. Klochkov,Konstantin Postnov,Peter Kretschmar,Katja Pottschmidt,Katja Pottschmidt,Frank Haberl,Richard E. Rothschild,Andrea Santangelo,Jörn Wilms,Ingo Kreykenbohm,Felix Fürst +13 more
TL;DR: In this paper, the cyclotron resonant scattering features (CRSF) were used to measure the magnetic field strength of a binary pulsar with magnetic fields on the order of several 1012 Gauss.
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Observational diversity of magnetized neutron stars.
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Polarized thermal emission from X-ray dim isolated neutron stars: the case of RX J1856.5−3754
TL;DR: In this paper, the polarization properties of thermal radiation from isolated, cooling neutron stars depend on both the emission processes at the surface and the effects of the magnetized vacuum which surrounds the star.
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