Magnetic Fields of Neutron Stars in X-Ray Binaries

Revnivtsev, M.; Mereghetti, S.

doi:10.1007/s11214-014-0123-x

Cited by 50 publications

(39 citation statements)

References 148 publications

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“…Gammie 1998;Begelman 2006). However, there has not been clear evidence of their presence in PDS (Revnivtsev & Mereghetti 2015). Moreover, at least for the accretion column, the timescales are most likely outside the frequency range we examine, so we consider the scenario outlined above more plausible.…”

Section: Transfer Functionmentioning

confidence: 92%

Evidence for the radiation-pressure dominated accretion disk in bursting pulsar GRO J1744−28 using timing analysis

Mönkkönen

Tsygankov

Mushtukov

et al. 2019

A&A

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The X-ray pulsar GRO J1744−28 is a unique source which shows both pulsations and type-II X-ray bursts, allowing studies of the interaction of the accretion disk with the magnetosphere at huge mass accretion rates exceeding 10 19 g s −1 during its super-Eddington outbursts. The magnetic field strength in the source, B ≈ 5 × 10 11 G, is known from the cyclotron absorption feature discovered in the energy spectrum around 4.5 keV. Here, we explore the flux variability of the source in context of interaction of its magnetosphere with the radiation-pressure dominated accretion disk. Particularly, we present the results of the analysis of noise power density spectra (PDS) using the observations of the source in 1996-1997 by the Rossi X-ray Timing Explorer (RXTE). Accreting compact objects commonly exhibit a broken power-law shape of the PDS with a break corresponding to the Keplerian orbital frequency of matter at the innermost disk radius. The observed frequency of the break can thus be used to estimate the size of the magnetosphere. We found, however, that the observed PDS of GRO J1744−28 differs dramatically from the canonical shape. Furthermore, the observed break frequency appears to be significantly higher than what is expected based on the magnetic field estimated from the cyclotron line energy. We argue that these observational facts can be attributed to the existence of the radiation-pressure dominated region in the accretion disk at luminosities above ∼2×10 37 erg s −1 . We discuss a qualitative model for the PDS formation in such disks, and show that its predictions are consistent with our observational findings. The presence of the radiation-pressure dominated region can also explain the observed weak luminosity-dependence of the inner radius, and we argue that the small inner radius can be explained by a quadrupole component dominating the magnetic field of the neutron star.

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Section: Transfer Functionmentioning

confidence: 92%

Evidence for the radiation-pressure dominated accretion disk in bursting pulsar GRO J1744−28 using timing analysis

Mönkkönen

Tsygankov

Mushtukov

et al. 2019

A&A

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“…So far, the CRSF has been detected from about 25 XBPs altogether, of which 15 are Be XBPs (e.g. Revnivtsev & Mereghetti 2015;Walter et al 2015). Therefore, focusing on Be XBPs will also satisfy the third requirement.…”

Section: Introductionmentioning

confidence: 99%

Correlation between the luminosity and spin-period changes during outbursts of 12 Be binary pulsars observed by the MAXI/GSC and the Fermi/GBM

Sugizaki

Mihara

Nakajima

et al. 2017

Publications of the Astronomical Society of Japan

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To observationally study spin-period changes of accreting pulsars caused by the accretion torque, the present work analyzes X-ray light curves of 12 Be binary pulsars obtained by the MAXI/GSC all-sky survey and their pulse periods measured by the Fermi/GBM pulsar project, both covering more than 6 years from 2009 August to 2016 March. The 12 objects were selected because they are accompanied by clear optical identification, and accurate measurements of surface magnetic fields. The luminosity L and the spin-frequency derivativesν, measured during large outbursts with L > ∼ 1 × 10 37 erg s −1 , were found to approximately follow the theoretical relations in the accretion torque models, represented byν ∝ L α (α ≃ 1), and the coefficient of proportionality betweenν and L α , agrees, within a factor of ∼ 3, with that proposed by Ghosh & Lamb (1979). In the course of the present study, the orbital elements of several sources were refined.

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“…3), together with the critical luminosity, L crit . B is the NS magnetic field in units of 10 12 G, z is the NS gravitational redshift (values taken fromRevnivtsev & Mereghetti 2015).…”

mentioning

confidence: 99%

An INTEGRAL overview of High-Mass X–ray Binaries: classes or transitions?

Sidoli

Paizis

2018

Monthly Notices of the Royal Astronomical Society

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We analyzed in a systematic way the public INTEGRAL observations spanning from December 2002 to September 2016, to investigate the hard X-ray properties of about 60 High Mass X-ray Binaries (HMXBs). We considered both persistent and transient sources, hosting either a Be star (Be/XRBs) or a blue supergiant companion (SgHMXBs, including Supergiant Fast X-ray Transients, SFXTs), a neutron star or a black hole. INTEGRAL X-ray light curves (18-50 keV), sampled at a bin time of about 2 ks, were extracted for all HMXBs to derive the cumulative distribution of their hard X-ray luminosity, their duty cycle, the range of variability of their hard X-ray luminosity. This allowed us to obtain an overall and quantitative characterization of the long-term hard X-ray activity of the HMXBs in our sample. Putting the phenomenology observed with INTEGRAL into context with other known source properties (e.g. orbital parameters, pulsar spin periods) together with observational constraints coming from softer X-rays (1-10 keV), enabled the investigation of the way the different HMXB subclasses behave (and sometimes overlap). For given source properties, the different sub-classes of massive binaries seem to cluster in a suggestive way. However, for what concerns supergiant systems (SgHMXBs versus SFXTs), several sources with intermediate properties exist, suggesting a smooth transition between the two sub-classes.

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Magnetic Fields of Neutron Stars in X-Ray Binaries

Cited by 50 publications

References 148 publications

Evidence for the radiation-pressure dominated accretion disk in bursting pulsar GRO J1744−28 using timing analysis

Evidence for the radiation-pressure dominated accretion disk in bursting pulsar GRO J1744−28 using timing analysis

Correlation between the luminosity and spin-period changes during outbursts of 12 Be binary pulsars observed by the MAXI/GSC and the Fermi/GBM

An INTEGRAL overview of High-Mass X–ray Binaries: classes or transitions?

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