Constraining the dipolar magnetic field of M82 X-2 by the accretion model

Chen, Wen-Cong

doi:10.1093/mnrasl/slw200

Cited by 11 publications

(4 citation statements)

References 44 publications

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“…Subsequently, more and more ULXPs were discovered but none of them was confirmed to be a magnetar (King & Lasota 2019). However, an interesting idea is that M82 X-2 is an accreting low magnetic field magnetar (Tong 2015;Tong & Wang 2019) with B ∼ 10 12 G (Chen 2017). This is in accord with the current view that the magnetars' ultrahigh fields decay on a timescale <10 5 -10 6 yr by Hall draft and Ohmic diffusion (Turolla et al 2015).…”

Section: Introductionsupporting

confidence: 54%

Are There Magnetars in High-mass X-Ray Binaries?*

Xu¹,

Li²,

Cui³

et al. 2022

Res. Astron. Astrophys.

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Magnetars form a special population of neutron stars with strong magnetic fields and long spin periods. About 30 magnetars and magnetar candidates known currently are probably isolated, but the possibility that magnetars are in binaries has not been excluded. In this work, we perform spin evolution of neutron stars with different magnetic fields in wind-fed high-mass X-ray binaries and compare the spin period distribution with observations, aiming to find magnetars in binaries. Our simulation shows that some of the neutron stars, which have long spin periods or are in widely-separated systems, need strong magnetic fields to explain their spin evolution. This implies that there are probably magnetars in high-mass X-ray binaries. Moreover, this can further provide a theoretical basis for some unclear astronomical phenomena, such as the possible origin of periodic fast radio bursts from magnetars in binary systems.

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Section: Introductionsupporting

confidence: 54%

Are There Magnetars in High-mass X-Ray Binaries?*

Xu¹,

Li²,

Cui³

et al. 2022

Res. Astron. Astrophys.

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“…Since the emergent radiation is multiply scattered in the accretion column walls, with the ordinary and extraordinary waves being transformed into one another, the effective scattering cross section in the standard X-ray band (E ∼ < 10 keV) can be appreciably smaller than σ T (Paczynski 1992). Introducing an anisotropy factor γ > 1, suggesting that the radiation intensity toward us is greater than the mean intensity by a factor of γ, from inequality (7) we finally obtain…”

Section: The Regimes Of Supercritical Accretionmentioning

confidence: 99%

“…Because of the weak magnetic field, the accretion disk almost reaches the neutron star surface and radiates in the same way as during super-Eddington accretion onto a black hole. In both cases, the limiting observed luminosity of ULX pulsars, L iso ∼ 10 41 erg s −1 , still cannot be explained and one has to appeal to a strong anisotropy of their radiation (dall 'Osso et al 2015;Chen 2017).…”

Section: Introductionmentioning

confidence: 99%

The nature of the bimodal luminosity distribution of ultraluminous X-ray pulsars

Гребенев

2017

Astron. Lett.

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The mechanism that can be responsible for the bimodal luminosity distribution of superEddington X-ray pulsars in binary systems is pointed out. The transition from the high to low state of these objects is explained by accretion flow spherization due to the radiation pressure at certain (high) accretion rates. The transition between the states can be associated with a gradual change in the accretion rate. The complex behavior of the recently discovered ultraluminous X-ray pulsars M 82 X-2, NGC 5907 ULX-1, and NGC 7793 P13 is explained by the proposed mechanism. The proposed model also naturally explains the measured spinup of the neutron star in these pulsars, which is slower than the expected one by several times.

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“…Physical properties of ULX pulsars are still open questions. Magnetic fields of M82 X-2 are ranging 10 9 G B 10 14 G in literatures [18,25,49,53,54,66,82].…”

Section: Ulx Pulsarsmentioning

confidence: 99%

High energy gamma rays from nebulae associated with extragalactic microquasars and ultra-luminous X-ray sources

Inoue

Lee

Tanaka

et al. 2017

Astroparticle Physics

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In the extragalactic sky, microquasars and ultra-luminous X-ray sources (ULXs) are known as energetic compact objects locating at off-nucleus positions in galaxies. Some of these objects are associated with expanding bubbles with a velocity of 80-250 km s −1 . We investigate the shock acceleration of particles in those expanding nebulae. The nebulae having fast expansion velocity 120 km s −1 are able to accelerate cosmic rays up to ∼ 100 TeV. If 10% of the shock kinetic energy goes into particle acceleration, powerful nebulae such as the microquasar S26 in NGC 7793 would emit gamma rays up to several tens TeV with a photon index of ∼ 2. These nebulae will be good targets for future Cherenkov Telescope Array observations given its sensitivity and angular resolution. They would also contribute to ∼ 7% of the unresolved cosmic gamma-ray background radiation at ≥ 0.1 GeV. In contrast, particle acceleration in slowly expanding nebulae 120 km s −1 would be less efficient due to ion-neutral collisions and result in softer spectra at 10 GeV.

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Constraining the dipolar magnetic field of M82 X-2 by the accretion model

Cited by 11 publications

References 44 publications

Are There Magnetars in High-mass X-Ray Binaries?*

Are There Magnetars in High-mass X-Ray Binaries?*

The nature of the bimodal luminosity distribution of ultraluminous X-ray pulsars

High energy gamma rays from nebulae associated with extragalactic microquasars and ultra-luminous X-ray sources

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