Luminosity Dependent Changes of Pulse Profiles in the X-ray Binary GX 1+4

Greenhill, J.; Storey, Michelle C.

doi:10.1071/as98254

Cited by 8 publications

(16 citation statements)

References 15 publications

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“…As regards the changes in the pulse profiles, many authors (see, e.g., Greenhill et al (1998) and references therein) showed that the profile clearly depends not only on the source intensity but also on the spin-up. According to IBIS data, the source pulse profile is single-peaked with a slight tendency for the separation into two subpeaks with increasing energy (Figs.…”

Section: Resultsmentioning

confidence: 99%

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

2009

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Abstract-We review the results of a timing analysis of the observations for ten bright X-ray pulsars (with fluxes >100 mCrab in the 20-100 keV energy band) that fell within the INTEGRAL field of view from 2003 to 2007. The dependence of the pulse profile on the energy and intrinsic source luminosity has been investigated; particular attention has been paid to searching for changes in the pulse profile near the cyclotron frequency. The dependence of the pulsed fraction for X-ray pulsars on their luminosity and energy band has been studied in detail for the first time.PACS numbers : 97.80. Ip; 97.60.Id; 95.75.Wx

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Section: Resultsmentioning

confidence: 99%

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

2009

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“…However, there is suggestion of some decrease in the pulsed fraction above 30 keV which maybe due to the morphology of the accretion column of the pulsar. The asymmetric nature of folded profiles in X-ray pulsars have been suggested to occur due to the distortion of the dipole magnetic field (Kraus et al 1995;Sasaki et al 2012) or higher-order multipole field components (Greenhill et al 1998) or the asymmetric nature of the accretion stream near the neutron star (Basko & Sunyaev 1976;Wang & Welter 1981;Miller 1996).…”

Section: Broadband Energy Resolved Pulse Profilesmentioning

confidence: 99%

Study of recent outburst in the Be/X-ray binary RX J0209.6−7427 with AstroSat: a new ultraluminous X-ray pulsar in the Magellanic Bridge?

Chandra

Roy

Agrawal

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the timing and spectral studies of RX J0209.6–7427 during its rare 2019 outburst using observations with the Soft X-ray Telescope (SXT) and Large Area X-ray Proportional Counter (LAXPC) instruments on the AstroSat satellite. Pulsations having a periodicity of 9.29 s were detected for the first time by the NICER mission in the 0.2–10 keV energy band and, as reported here, by AstroSat over a broad energy band covering 0.3–80 keV. The pulsar exhibits a rapid spin-up during the outburst. Energy resolved folded pulse profiles are generated in several energy bands in 3–80 keV. To the best of our knowledge this is the first report of the timing and spectral characteristics of this Be binary pulsar in hard X-rays. There is suggestion of evolution of the pulse profile with energy. The energy spectrum of the pulsar is determined and from the best-fitting spectral values, the X-ray luminosity of RX J0209.6−7427 is inferred to be 1.6 × 1039 erg s−1. Our timing and spectral studies suggest that this source has features of an ultraluminous X-ray pulsar in the Magellanic Bridge. Details of the results are presented and discussed in terms of the current ideas.

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“…Dips are the sharp drops in intensity over a narrow phase range of ∆φ ≈ 0.1 (see e.g., Greenhill et al, 1998;Giles et al, 2000;Galloway et al, 2001;Devasia et al, 2010Devasia et al, , 2011aDevasia et al, 2011b;Usui et al, 2012;. The depth of a dip can attain a very high value, 80-100% of the pulse maximum (Giles et al, 2000).…”

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confidence: 99%

Post-flare formation of the accretion stream and a dip in pulse profiles of LMC X–4

Beri

Paul

2017

New Astronomy

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We report here a pulse profile evolution study of an accreting X-ray pulsar LMC X-4 during and after the large X-ray flares using data from the two observatories XMM-Newton and RXTE. During the flares, the pulse profiles were found to have a significant phase offset in the range of 0.2-0.5 compared to the pulse profiles immediately before or after the flare. Investigating the pulse profiles for about 10 5 seconds after the flares, it was found that it takes about 2000-4000 seconds for the modified accretion column to return to its normal structure and formation of an accretion stream that causes a dip in the pulse profile of LMC X-4. We have also carried out pulse phase resolved spectroscopy of LMC X-4 in narrow phase bins using data from EPIC-pn and spectroscopically confirmed the pulsating nature of the soft spectral component, having a pulse fraction and phase different from that of the power-law component.

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Luminosity Dependent Changes of Pulse Profiles in the X-ray Binary GX 1+4

Cited by 8 publications

References 15 publications

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

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

Study of recent outburst in the Be/X-ray binary RX J0209.6−7427 with AstroSat: a new ultraluminous X-ray pulsar in the Magellanic Bridge?

Post-flare formation of the accretion stream and a dip in pulse profiles of LMC X–4

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