Hard X‐Ray Lags in GRO J1719−24

Hooft, F. van der; Kouveliotou, C.; Paradijs, J.A. van; Pačiesas, W. S.; Lewin, W. H. G.; Klis, M. van der; Crary, David; Finger, Mark H.; Harmon, B. A.; Zhang, S.N.

doi:10.1086/307346

Cited by 9 publications

(11 citation statements)

References 17 publications

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“…A general softening of the spectrum, consistent with this geometry, was also observed, and was seen previously in GS 1354−64 by Kitamoto et al (1990). A similar increase in frequency of low‐frequency QPOs was discovered during an outburst of the X‐ray transient GRO J1719−24 by Van der Hooft et al (1996). If the increasing frequencies of the QPOs really do relate to the inner disc, then it is interesting to note that the inner disc radius does not appear to increase again during the decay from outburst.…”

Section: Results and Analysissupporting

confidence: 87%

“…Sunyaev et al 1993), GRO J1719−24 (e.g. Van der Hooft et al 1996) and GS 2023+338, although in the last case it is possible that the system was in a soft but absorbed state at its peak, then returning to the low/hard state (Życki, Done & Smith 1999).…”

Section: Results and Analysismentioning

confidence: 99%

“…Although these objects are frequently referred to as soft X‐ray transients on account of their ultrasoft X‐ray spectra during the outbursts, an increasing number of their outbursts do not show the soft component (e.g., GRO J1719−24; Van der Hooft et al 1996). Instead, the power‐law component dominates the energy spectrum, reminiscent of the low/hard X‐ray state of the persistent source Cyg X‐1.…”

Section: Introductionmentioning

confidence: 99%

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The 1997 hard-state outburst of the X-ray transient GS 1354-64/BW Cir

Brocksopp

Jonker

Fender

et al. 2001

Monthly Notices of the Royal Astronomical Society

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We present observations of the 1997 outburst of the X‐ray transient GS 1354−64 (BW Cir) at X‐ray, optical and, for the first time, radio wavelengths; our results include upper limits to the linear and circular polarization for the radio data. The X‐ray outburst was unusual in that the source remained in the low/hard X‐ray state throughout; the X‐ray peak was also preceded by at least one optical outburst, suggesting that it was an ‘outside‐in’ outburst – similar to those observed in dwarf novae systems, although possibly taking place on a viscous time‐scale in this case. It therefore indicates that the optical emission was not dominated by the reprocessing of X‐rays, but that instead we see the instability directly. While the radio source was too faint to detect any extended structure, spectral analysis of the radio data and a comparison with other similar systems suggest that mass ejections, probably in the form of a jet, took place and that the emitted synchrotron spectrum may have extended as far as infrared wavelengths. Finally, we compare this 1997 outburst of GS 1354−64 with possible previous outbursts and also with other hard‐state objects, both transient and persistent. It appears that a set of characteristics – such as a weak, flat‐spectrum radio jet, a mHz QPO increasing in frequency, a surprisingly high optical/X‐ray luminosity ratio, and the observed optical peak preceding the X‐ray peak – may be common to all hard‐state X‐ray transients.

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Section: Results and Analysissupporting

confidence: 87%

Section: Results and Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The 1997 hard-state outburst of the X-ray transient GS 1354-64/BW Cir

Brocksopp

Jonker

Fender

et al. 2001

Monthly Notices of the Royal Astronomical Society

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“…the spectra is puzzling. It is also important that for all the candidates in Set A, the time lag in hard X-ray with respect to the softer Xray is around 0.1 − 1s (van der Hooft et al 1999), which point to an extended region of hard X-ray emission region. It is possible that these two properties of Set A candidates are related.…”

Section: Spectral Properties Of Galactic Black Holes In γ-Raysmentioning

confidence: 99%

Spectral Properties of Black Holes in Gamma Rays

Chakrabarti

2005

Astrophys Space Sci

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Abstract. Black holes are the most compact objects in the universe. Therefore, matter accreting onto is likely to radiate photons of energy comparable to very high gravitational potential energy. We discuss the nature of the emitted radiation in Xrays and gamma-rays from black hole candidates. We present theoretical solutions which comprise both Keplerian and sub-Keplerian components and suggest that shocks in accretion and outflows may play a major role in producing this spectra.

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“…The compact object is believed to be a stellarmass black hole of mass ∼ 4.9M⊙, located at a distance of ∼ 2.0-2.8 kpc. The only observed historical major outburst from GRS 1716-249 coincided with its discovery in 1993, which was later studied in detail by van der Hooft et al (1996), to investigate the nature of its temporal variability. During the entire 80 days of its outburst, the authors witnessed a QPO at ν ∼ 0.04 Hz at the beginning of the observations, which gradually shifted to 0.3 Hz at the end.…”

Section: Introductionmentioning

confidence: 99%

Re-awakening of GRS 1716–249 after 23 yr, observed by Swift/XRT and NuSTAR

Bharali

Chandra

Chauhan

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In this work, we present a spectral and temporal analysis of Swift/XRT and NuS-TAR observations of GRS 1716-249 during its recent 2016-2017 outburst. This low mass X-ray binary underwent an extraordinary outburst after a long quiescence of 23 years, since its last major outburst in 1993. The source was observed over two different epochs during 2017 April, 07 and 10. The best fit joint spectral fitting in the energy range 0.5 − 79.0 keV indicates that the spectrum is best described by relatively cold, weak disk blackbody emission, dominant thermal Comptonization emission, and a relativistically broadened fluorescent iron Kα emission line. We observed a clear indication of a Compton hump around 30 keV. We also detected an excess feature of ∼ 1.3 keV. Assuming a lamp-post geometry of the corona, we constrained the inner disk radius for both observations to 11.92 +8.62 −11.92 R ISCO (i.e., an upper limit) and 10.39 +9.51 −3.02 R ISCO (where R ISCO ≡ radius of the innermost stable circular orbit) for the first epoch (E1) and second epoch (E2), respectively. A significant (∼ 5σ) type−C quasi-periodic oscillation (QPO) at 1.20±0.04 Hz is detected for the first time for GRS 1716-249, which drifts to 1.55 ± 0.04 Hz (∼ 6σ) at the end of the second observation. The derived spectral and temporal properties show a positive correlation between the QPO frequency and the photon index.

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Hard X‐Ray Lags in GRO J1719−24

Cited by 9 publications

References 17 publications

The 1997 hard-state outburst of the X-ray transient GS 1354-64/BW Cir

The 1997 hard-state outburst of the X-ray transient GS 1354-64/BW Cir

Spectral Properties of Black Holes in Gamma Rays

Re-awakening of GRS 1716–249 after 23 yr, observed by Swift/XRT and NuSTAR

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