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Remillard, Stephen K.; Abdelmonem, A.; Radzikowski, Piotr O.; Lazzaro, Nick D.; Applegate, D.S.

doi:10.1023/a:1007880105379

Cited by 25 publications

(11 citation statements)

References 3 publications

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“…XTE J1650-500 was first discovered by RXTE during its 2001 outburst (Remillard 2001). We adopt 5.1 M for the mass of the black hole, as estimated by Slanỳ & Stuchlik (2008) and within the mass limit estimated by Orosz et al (2004) (2.7 < M BH < 7.3 M ).…”

Section: Xte J1650-500mentioning

confidence: 99%

Evidence for an expanding corona based on spectral-timing modelling of multiple black hole X-ray binaries

Cao

Lucchini

Markoff

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Galactic black hole X-ray binaries (BHXBs) provide excellent laboratories to study accretion, as their relatively quick evolution allows us to monitor large changes in the in-flowing and/or out-flowing material over human timescales. However, the details of how the inflow-outflow coupling evolves during a BHXB outburst remain an area of active debate. In this work we attempt to probe the physical changes underlying the system evolution, by performing a systematic analysis of the multi-wavelength data of three BHXB sources: XTE J1752-223, MAXI J1659-152, and XTE J1650-500, during hard and hard-intermediate states. Using the power spectral hue which characterises the X-ray variability properties, we identify several clusters of BHXB epochs and perform the joint multi-wavelength spectral modelling to test their commonality with a physical jet model. Under the assumption that the corona is related to the base of the jet, we find that the power spectral hue traces the variation of the coronal radius (from ∼10Rg − ∼ 40Rg) in multiple BHXBs at hard and hard-intermediate states, and that the data are consistent with moderately truncated accretion discs (<25Rg) during hard-intermediate states. We also find that all epochs of low disc reflection have high hue located near the hard-intermediate to soft-intermediate state transition, indicating that in these states the vertical extent of the corona and/or its bulk speed are increasing. Our results link the geometrical similarity in the corona among multiple BHXB sources to their timing characteristics, and probe the corona responding to the disc-jet interactions at hard and intermediate states during outbursts.

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Section: Xte J1650-500mentioning

confidence: 99%

Evidence for an expanding corona based on spectral-timing modelling of multiple black hole X-ray binaries

Cao

Lucchini

Markoff

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…The Galactic X-ray binary system XTE J1650Ϫ500 entered a quiescent regime following the 2001-2002 outburst that led to its discovery with the Rossi X-Ray Timing Explorer (Remillard 2001). Observations conducted with XMM-Newton and BeppoSAX in late 2001, right after the outburst peak, revealed a broad, asymmetric Fe Ka emission line, interpreted as due to a irradiation of the inner accretion disk around a rapidly spinning Kerr BH (Miller et al 2002;Miniutti et al 2004; see Done & Gierlinski 2006 for a different interpretation).…”

Section: ϫ1 ϫ6mentioning

confidence: 99%

Chandra Detection of XTE J1650-500 in Quiescence and the Minimum Luminosity of Black Hole X-Ray Binaries

Gallo

Homan

Jonker

et al. 2008

ApJ

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The Galactic black hole X-ray binary XTE J1650-500 entered a quiescent regime following the decline from the 2001-2002 outburst that led to its discovery. Here we report on the first detection of its quiescent counterpart in a 36 ks observation taken in 2007 July with the Chandra X-ray Observatory. The inferred 0.5-10 keV unabsorbed flux is in the range 2.5-5.0 × 10 −15 erg s −1 cm −2 . Notwithstanding large distance uncertainties, the measured luminosity is comparable to that of the faintest detected black hole X-ray binaries, all having orbital periods close to the expected bifurcation period between jand n-driven low-mass X-ray binaries. This suggests that a few 10 30 erg s −1 might be a limiting luminosity value for quiescent black holes.

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“…We must press hard to obtain further observations of black hole masses in order to fully pursue these opportunities. XTE J1650À500 ( hereafter J1650) was discovered by the Rossi X-Ray Timing Explorer (RXTE ) on 2001 September 5 ( Remillard 2001) and subsequently reached a peak X-ray intensity of 0.5 crab. Based on subsequent observations, J1650 was established as a strong black hole candidate based on its X-ray spectrum and variability in the X-ray light curve ( Markwardt et al 2001;Revnivtsev & Sunyaev 2001;Wijnands et al 2001).…”

Section: Introductionmentioning

confidence: 99%

Orbital Parameters for the Black Hole Binary XTE J1650−500

Orosz

McClintock

Remillard

et al. 2004

ApJ

107

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We present R-band photometry of the X-ray transient and candidate black hole binary XTE J1650À500 obtained between 2003 May and August with the 6.5 m Clay telescope. A timing analysis of these data reveals a photometric period of 0:3205 AE 0:0007 days (i.e., 7.63 hr) with a possible alias at 0.3785 days (9.12 hr). Our photometry completely rules out the previously published spectroscopic period of 0.212 days (5.09 hr). Consequently, we reanalyzed the 15 archival ESO VLT spectra (obtained 2002 June by Sanchez-Fernandez et al.) that were the basis of the previously published spectroscopic period. We used a ''rest-frame search'' technique that is well suited for cases in which the signal-to-noise ratio of individual spectra is low. For each of roughly 1.1 million binary ephemerides, we summed all of the spectra in a trial rest frame of the secondary star, and each rest-frame spectrum was cross-correlated against a template spectrum. We then searched for the set of orbital parameters that produced the strongest cross-correlation value. The results confirmed the photometric period of 0.3205 days and ruled out the alias period near 0.38 days. The best value for the velocity semiamplitude of the companion star is K 2 ¼ 435 AE 30 km s À1 , and the corresponding optical mass function is f (M ) ¼ 2:73 AE 0:56 M . The spectral type of the companion star is not well constrained because we only have six template spectra available to us. The K4 V template provides the best match; next-best matches are provided by the G5 V and K2 III templates. We also find that the accretion disk dominates the light in the R band where the disk fraction is 80% or higher, although this value should be treated with caution owing to the poor signal-to-noise ratio and the limited number of templates. The amplitude of the phased R-band light curve is 0.2 mag, which gives a lower limit to the inclination of 50 AE 3 in the limiting case of no contribution to the R-band light curve from the accretion disk. If the mass ratio of XTE J1650À500 is similar to the mass ratios of other black hole binaries, such as A0620À00 or GRS 1124À683 (e.g., Q k10), then our lower limit to the inclination gives an upper limit to the mass of the black hole in XTE J1650À500 of M 1 P 7:3 M . However, the mass can be considerably lower if the R-band flux is dominated by the accretion disk. For example, if the accretion disk does contribute 80% of the flux, as our preliminary results suggest, then the black hole mass would be only about 4 M .

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Cited by 25 publications

References 3 publications

Evidence for an expanding corona based on spectral-timing modelling of multiple black hole X-ray binaries

Evidence for an expanding corona based on spectral-timing modelling of multiple black hole X-ray binaries

Chandra Detection of XTE J1650-500 in Quiescence and the Minimum Luminosity of Black Hole X-Ray Binaries

Orbital Parameters for the Black Hole Binary XTE J1650−500

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