Accreting Strongly Magnetized Neutron Stars: X-ray Pulsars

Mushtukov, Alexander; Tsygankov, Sergey

doi:10.1007/978-981-16-4544-0_104-1

Cited by 5 publications

(2 citation statements)

References 212 publications

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“…When the angle θ R = 80°(the angle of the magnetic axis to the rotational axis) and the inclination of the rotation axis i = 50°, the simulated pulse profile (Figure 12(b) in the work of Inoue 2020) is similar to the structure of the main and minor peaks of Swift J0243.6+6124. The radiation of the fan beam is directed toward the neutron star due to the electron scattering effect and gravitational bending (Inoue 2020;Mushtukov & Tsygankov 2023). Therefore, we only draw the main radiation distribution of the fan beam (the yellow light on the inner disk in Figures 6(f) and (g)).…”

Section: Modulated Iron Line Featurementioning

confidence: 99%

Pulsed Iron Line Emission from the First Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124

Xiao,

Xu,

et al. 2024

ApJ

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We report the phase-resolved spectral results of the first Galactic pulsating ultraluminous X-ray source (PULX) Swift J0243.6+6124, modeling its 2017–2018 outburst peak using data collected by the Hard X-ray Modulation Telescope (Insight-HXMT). The broad energy coverage of Insight-HXMT allows us to obtain a more accurate spectral continuum to reduce the coupling of broad iron line profiles with other components. We use three different continuum spectrum models but obtain similar iron line results. For the first time, we detect the pulse characteristics of the broad iron line in a PULX. The variation in the width and intensity of this iron line with σ ∼ 1.2–1.5 keV has a phase offset of about 0.25 from the pulse phase. We suggest that the uneven irradiation of the thick inner disk by the accretion column produces the modulated variation of the broad iron line. In addition, the nonpulsed narrow line is suggested to come from the outer disk region.

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Section: Modulated Iron Line Featurementioning

confidence: 99%

Pulsed Iron Line Emission from the First Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124

Xiao,

Xu,

et al. 2024

ApJ

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“…Accretion-powered X-ray pulsars (XRPs) are intriguing systems that enable the study of complex radiative processes in the presence of strong magnetic fields (for review see Mushtukov & Tsygankov 2023). The accreting material is entrained from the surrounding accretion disk by the strong magnetic field and then channeled onto a magnetic pole of the neutron star (NS), forming an accretion column (AC).…”

Section: Introductionmentioning

confidence: 99%

Theoretical Analysis of the RX J0209.6−7427 X-Ray Spectrum during a Giant Outburst

West,

Becker,

Vasilopoulos

2024

ApJL

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We model the spectral formation occurring in the binary X-ray pulsar (XRP) RX J0209.6−7427 during the 2019 super-Eddington outburst. Using a theoretical model previously developed by the authors, we are able to produce spectra that closely resemble the phase-averaged X-ray spectra observed using the Nuclear Spectroscopic Telescope Array and Insight-HXMT during low- and high-luminosity states of the outburst, respectively. The theoretical model simulates the accretion of fully ionized gas in a dipole magnetic field and includes a complete description of the radiation hydrodynamics, matter distribution, and spectral formation. Type II X-ray outbursts provide an opportunity to study accretion over a large range of luminosities for the same neutron star. The analysis performed here represents the first time both the outburst low and high states of an accretion-powered XRP are modeled using a physics-based model rather than standard phenomenological fitting with arbitrary mathematical functions. We find that the outer polar cap radius remains constant and the column is more fully filled with increasing luminosity, Comptonized bremsstrahlung dominates the formation of the phase-averaged X-ray spectrum, and a negative correlation exists between cyclotron centroid energy and luminosity, as expected. The super-Eddington nature of the outburst is rendered possible owing to the low scattering cross section for photons propagating parallel to the magnetic field. We also find that emission through the column top dominates in both the low and high states, implying that the pulse profiles should have a roughly sinusoidal shape, which agrees with observed properties of ultraluminous XRPs.

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Fundamental Physics with Neutron Stars

Nättilä,

Kajava

2024

Handbook of X-Ray and Gamma-Ray Astrophysics

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Accreting Strongly Magnetized Neutron Stars: X-ray Pulsars

Cited by 5 publications

References 212 publications

Pulsed Iron Line Emission from the First Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124

Pulsed Iron Line Emission from the First Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124

Theoretical Analysis of the RX J0209.6−7427 X-Ray Spectrum during a Giant Outburst

Fundamental Physics with Neutron Stars

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