Discovery of the Orbit of the X-ray pulsar OAO 1657-415

Chakrabarty, Deepto; Grunsfeld, J. M.; Prince, Thomas A.; Bildsten, Lars; Finger, Mark H.; Wilson, Robert B.; Fishman, G. J.; Meegan, C.; Pačiesas, W. S.

doi:10.1086/186715

Cited by 74 publications

(140 citation statements)

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“…OAO 1657−415 is unique among the known HMXBs as it is believed to be a wind-fed system for most of the time, and to only sporadically undergo episodes of accretion from a temporary disk. Since the binary is too wide for Roche-lobe overflow to occur, this may provide the first clear evidence that winds in HMXBs possess sufficient angular momentum to form accretion disks (see, e.g., Bildsten et al 1997;Chakrabarty et al 1993). Additional information on the ten sources can be found in Liu et al (2006).…”

Section: Ten Eclipsing Hmxbsmentioning

confidence: 95%

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Ephemeris, orbital decay, and masses of ten eclipsing high-mass X-ray binaries

Falanga

Bozzo

Lutovinov

et al. 2015

A&A

180

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We update the ephemeris of the eclipsing high-mass X-ray binary (HMXB) systems LMC X-4, Cen X-3, 4U 1700-377, 4U 1538-522, SMC X-1, IGR J18027-2016, Vela X-1,IGR J17252-3616, XTE J1855-026, and OAO 1657-415 with the help of more than ten years of monitoring these sources with the All Sky Monitor onboard RXTE and with the Integral Soft Gamma-Ray Imager onboard INTEGRAL. These results are used to refine previous measurements of the orbital period decay of all sources (where available) and provide the first accurate values of the apsidal advance in Vela X-1 and 4U 1538-522. Updated values for the masses of the neutron stars hosted in the ten HMXBs are also provided, as well as the long-term light curves folded on the best determined orbital parameters of the sources. These light curves reveal complex eclipse ingresses and egresses that are understood mostly as being caused by accretion wakes. Our results constitute a database to be used for population and evolutionary studies of HMXBs and for theoretical modeling of long-term accretion in wind-fed X-ray binaries.

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Section: Ten Eclipsing Hmxbsmentioning

confidence: 95%

“…Clark et al (1988), (c) Rubin et al (1996), (d) van Kerkwijk et al (1995a), (e) Hill et al (2005), ( f ) Corbet & Mukai (2002), (g) van Kerkwijk et al (1995b), (h) Corbet et al (2005), (i) Chakrabarty et al (1993). Table 7.…”

Section: Masses Of the Ten Neutron Starsunclassified

Ephemeris, orbital decay, and masses of ten eclipsing high-mass X-ray binaries

Falanga

Bozzo

Lutovinov

et al. 2015

A&A

180

265

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“…(1) Chakrabarty et al (1993); (2) Cherepashchuk et al (2005); (3) Sadakane et al (1985); (4) Notes. L x is the X-ray luminosity calculated using respective count rates and source distances listed in Table 1.…”

Section: Sourcesmentioning

confidence: 99%

Viscous timescale in high mass X-ray binaries

Icdem

Baykal

2011

A&A

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Context. Low mass X-ray binaries are found to have very low frequency breaks in their power density spectra. The power density spectra below these breaks are nearly in white noise structure and at higher frequencies approximately follow the P ν ∝ ν −1.3 law. Aims. To determine whether high mass X-ray binary power density spectra have similar properties and the findings for low mass X-ray binaries are also valid for high mass binaries, we analyzed the time series of high mass X-ray binary sources produced by All Sky Monitor of Rossi X-ray Timing Explorer. Methods. We obtained the power density spectra of the high mass X-ray binaries using the cosine transform of autocorrelation function. Results. We identified break frequencies for seven sources, namely OAO 1657-415, SS 433, Vela X-1, SMC X-1, 4U 1700-377, GX 301-2, and LMC X-1. The normalized break frequencies with respect to the orbital frequency ( f break / f orbit ) for sources OAO 1657-415, SS 433, SMC X-1 and LMC X-1 are consistent with those of Roche lobe overflow systems. The other high mass X-ray binary systems, Vela X-1, GX 301-2, and 4U 1700-377, however, have larger break frequency ratios, f break / f orb , which are indicative of short viscous times. These are all wind-accreting sources and the stellar winds in the systems allow the formation of only short radius discs. Consequently, we qualitatively distinguished the Roche lobe overflow binaries from the wind accreting system by comparing their normalized break frequencies.

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“…BATSE con rms this orbital decay Finger et al 1993 , which is thought to b edue to the tidal interaction of the neutron star with its companion. Chakrabarty et al 1993 , making it the seventh eclipsing X-ray pulsar discovered. The intrinsic spin frequency history reveals strong, stochastic variability and alternating episodes of steady spin-up and spin-down lasting 10 200 d, similar to what is seen in Cen X-3.…”

Section: Low-mass Systemsmentioning

confidence: 99%

“…The intrinsic spin frequency history reveals strong, stochastic variability and alternating episodes of steady spin-up and spin-down lasting 10 200 d, similar to what is seen in Cen X-3. Although the companion remains unidenti ed, it is inferred to b ean OB supergiant from the neutron-star orbit Table 3 and eclipse duration Chakrabarty et al 1993. Chakrabarty et al 1993 measured the binary orbital parameters using BATSE data spanning 1991 April 24 to 1992 July 23 MJD 48370 48460 .…”

Section: Low-mass Systemsmentioning

confidence: 99%

Observations of accreting pulsars

Prince

Bildsten

Chakrabarty

et al. 1994

AIP Conference Proceedings

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We summarize ve years of continuous monitoring of accretion-powered pulsars with the Burst and Transient Source Experiment BATSE on the Compton Gamma Ray Observatory. Our 20 70 keV observations have determined or re ned the orbital parameters of 13 binaries, discovered 5 new transient accreting pulsars, measured the pulsed ux history during outbursts of 12 transients GRO J1744 28, 4U 0115+634, GRO J1750 27, GS 0834 430, 2S 1417 624, GRO J1948+32, EXO 2030+375, GRO J1008 57, A 0535+26, GRO J2058+42, 4U 1145 619 and A 1118 616 , and also measured the accretion torque history of during outbursts of 6 of those transients whose orbital parameters were also known. We have also continuously measured the pulsed ux and spin frequency for eight persistently accreting pulsars Her X-1, Cen X-3, Vela X-1, OAO 1657 415, GX 301 2, 4U 1626 67, 4U 1538 52, and GX 1+4 . Because of their continuity and uniformity over a long baseline, BATSE observations have provided new insights into the long-term behavior of accreting magnetic stars. We have found that all accreting pulsars show stochastic variations in their spin frequencies and luminosities, including those displaying secular spin-up or spin-down on long time scales, blurring the conventional distinction b e t w een disk-fed and wind-fed binaries. Pulsed ux and accretion torque are strongly correlated in outbursts of transient accreting pulsars, but uncorrelated, or even anticorrelated, in persistent sources. We describe daily folded pulse pro les, frequency, and ux measurements that are available through the Compton Observatory Science Support Center at NASA-Goddard Space Flight Center.

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Discovery of the Orbit of the X-ray pulsar OAO 1657-415

Cited by 74 publications

References 0 publications

Ephemeris, orbital decay, and masses of ten eclipsing high-mass X-ray binaries

Ephemeris, orbital decay, and masses of ten eclipsing high-mass X-ray binaries

Viscous timescale in high mass X-ray binaries

Observations of accreting pulsars

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