Timing characteristics of the hard X-ray emission from bright X-ray pulsars based on INTEGRAL data

Lutovinov, A.; Tsygankov, S.

doi:10.1134/s1063773709070019

Cited by 101 publications

(110 citation statements)

References 46 publications

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“…5). At higher energies one can see the gradual increase of the pulsed fraction, typical for the majority of X-ray pulsars (Lutovinov & Tsygankov 2009). …”

Section: Timing Analysismentioning

confidence: 92%

NuSTARobservations of the supergiant X-ray pulsar IGR J18027−2016: accretion from the stellar wind and possible cyclotron absorption line

Lutovinov

Tsygankov

Постнов

et al. 2016

Mon. Not. R. Astron. Soc.

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We report on the first focused hard X-ray view of the absorbed supergiant system IGR J18027-2016 performed with the NuSTAR observatory. The pulsations are clearly detected with a period of P spin = 139.866(1) s and a pulse fraction of about 50-60% at energies from 3 to 80 keV. The source demonstrates an approximately constant X-ray luminosity on a time scale of more than dozen years with an average spin-down rate oḟ P ≃ 6×10 −10 s s −1 . This behaviour of the pulsar can be explained in terms of the wind accretion model in the settling regime. The detailed spectral analysis at energies above 10 keV was performed for the first time and revealed a possible cyclotron absorption feature at energy ∼ 23 keV. This energy corresponds to the magnetic field B ≃ 3×10 12G at the surface of the neutron star, which is typical for X-ray pulsars.

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“…5). At higher energies one can see the gradual increase of the pulsed fraction, typical for the majority of X-ray pulsars (Lutovinov & Tsygankov 2009). …”

Section: Timing Analysismentioning

confidence: 92%

NuSTARobservations of the supergiant X-ray pulsar IGR J18027−2016: accretion from the stellar wind and possible cyclotron absorption line

Lutovinov

Tsygankov

Постнов

et al. 2016

Mon. Not. R. Astron. Soc.

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“…For certain pulse phases, the inner parts of the column are obscured by the neutron star, and we can see only the outer, relatively cool parts, while a larger part of the column is seen at other phases. The pulse fraction is also expected to decrease with the increase in the column height and therefore with the source luminosity, which is indeed the case for GX 301−2 (Lutovinov & Tsygankov 2009). …”

Section: Implications Of the Strong Magnetic Fieldmentioning

confidence: 99%

Is there a highly magnetized neutron star in GX 301–2?

Doroshenko

Santangelo

Suleimanov

et al. 2010

A&A

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We present the results of an in-depth study of the long-period X-ray pulsar GX 301−2. Using archival data of INTEGRAL, RXTE ASM, and CGRO BATSE, we study the spectral and timing properties of the source. Comparison of our timing results with previously published work reveals a secular decay of the orbital period at a rate of −3.25 × 10 −5 d yr −1 , which is an order of magnitude faster than for other known systems. We argue that this is probably result either of the apsidal motion or of gravitational coupling of the matter lost by the optical companion with the neutron star, although current observations do not allow us to distinguish between those possibilities. We also propose a model to explain the observed long pulse period. We find that a very strong magnetic field B ∼ 10 14 G can explain the observed pulse period in the framework of existing models for torques affecting the neutron star. We show that the apparent contradiction with the magnetic field strength B CRSF ∼ 4 × 10 12 G derived from the observed cyclotron line position may be resolved if the line formation region resides in a tall accretion column of height ∼2.5-3 R NS . The color temperature measured from the spectrum suggests that such a column may indeed be present, and our estimates show that its height is sufficient to explain the observed cyclotron line position.

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“…In a simple toy model this can be explained by a change in altitude of the X-ray producing region in the accretion column (Lutovinov & Tsygankov 2009). Such a change would also be visible in a change of the energy of the CRSF (Suchy et al 2011;Doroshenko et al 2010).…”

Section: Accretion During the Off-statementioning

confidence: 99%

Study of the many fluorescent lines and the absorption variability in GX 301−2 withXMM-Newton

Fürst¹,

Suchy

Kreykenbohm³

et al. 2011

A&A

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We present an in-depth study of the high mass X-ray binary (HMXB) GX 301−2 during its pre-periastron flare using data from the XMM-Newton satellite. The energy spectrum shows a power law continuum absorbed by a large equivalent hydrogen column on the order of 10 24 cm −2 and a prominent Fe Kα fluorescent emission line. Besides the Fe Kα line, evidence for Fe Kβ, Ni Kα, Ni Kβ, S Kα, Ar Kα, Ca Kα, and Cr Kα fluorescent lines is found. The observed line strengths are consistent with fluorescence in a cold absorber. This is the first time that Cr Kα is seen in emission in the X-ray spectrum of a HMXB. In addition to the modulation by the strong pulse period of ∼685 s the source is highly variable and shows different states of activity. We perform time-resolved as well as pulse-to-pulse resolved spectroscopy to investigate differences between these states of activity. We find that fluorescent line fluxes are strongly variable and generally follow the overall flux. The N H value is variable by a factor of 2, but not correlated to continuum normalization. We find an interval of low flux in the light curve in which the pulsations cease almost completely, without any indication of an increasing absorption column. We investigate this dip in detail and argue that it is most likely that during the dip the accretion ceased and the afterglow of the fluorescent iron accounted for the main portion of the X-ray flux. A similar dip was found earlier in RXTE data, and we compare our findings to these results.

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Timing characteristics of the hard X-ray emission from bright X-ray pulsars based on INTEGRAL data

Cited by 101 publications

References 46 publications

NuSTARobservations of the supergiant X-ray pulsar IGR J18027−2016: accretion from the stellar wind and possible cyclotron absorption line

NuSTARobservations of the supergiant X-ray pulsar IGR J18027−2016: accretion from the stellar wind and possible cyclotron absorption line

Is there a highly magnetized neutron star in GX 301–2?

Study of the many fluorescent lines and the absorption variability in GX 301−2 withXMM-Newton

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