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Long-term evolutions of the cyclotron line energies in Her X-1, Vela X-1 and Cen X-3 as observed with Swift/BAT

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arxiv 1901.07269 v1 pith:S6XFHVQE submitted 2019-01-22 astro-ph.HE hep-ph

Long Ji , Ruediger Staubert , Lorenzo Ducci , Andrea Santangelo , Shu Zhang , Zhi Chang This is my paper · ORCID
classification astro-ph.HEhep-ph
keywords energylong-termvelacrsfcyclotronlineswiftcentroid
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We study the long-term evolution of the centroid energy of cyclotron lines - often referered to as Cyclotron Resonance Scattering Features (CRSF) - in Her X-1, Vela X-1 and Cen X-3, using survey observations of the Burst Alert Telescope (BAT) onboard Swift. We find a significant decrease of the fundamental CRSF energy in Her X-1 and the first harmonic line energy in Vela X-1, since the launch of Swift in 2004 and until 2010 and 2012, respectively.In both sources the decreases stopped at some time, with a quite stable centroid energy thereafter. Unlike in Her X-1 and Vela X-1, the CRSF energy in Cen X-3 does not show a long-term decrease. It is observed not to change for at least the past 14 years. The long-term variation of the line energy is a direct way to investigate the magnetic field structure in the polar regions of pulsars. Our results may stimulate the development of theoretical models, especially regarding to how the accreted mass accumulates in the accretion mound or how the magnetic field distorts around the polar cap.

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Cited by 2 Pith papers

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  1. Real-time observations of the transition to the quiescent state in an accreting magnetised neutron star: No propeller required?

    astro-ph.HE 2026-08 conditional novelty 6.0 of 10

    First high-cadence observation of an X-ray pulsar transition to quiescence shows a gradual exponential fade consistent with the disc instability model, without requiring the propeller effect.

  2. X-Ray Views of Galactic Accreting Pulsars in High-Mass X-Ray Binaries

    astro-ph.HE 2024-12 accept novelty 1.0 of 10

    A concise review of the timing, spectral, and polarization properties of accreting X-ray pulsars in high-mass X-ray binaries, including recent IXPE results.

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