Multiwavelength observations of the black hole transient Swift J1745−26 during the outburst decay

Kalemci, Emrah; Arabacı, M. Özbey; Güver, T.; Russell, D. M.; Tomsick, John A.; Wilms, J.; Weidenspointner, G.; Kuulkers, E.; Falanga, M.; Dinçer, Tolga; Drave, S. P.; Belloni, T.; Coriat, M.; Lewis, Fraser; Muñoz-Darias, T.

doi:10.1093/mnras/stu1851

Cited by 14 publications

(17 citation statements)

References 61 publications

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“…This would suggest that the overall mass-transfer rate during the outburst is not the only parameter involved in the "failed" state transition behavior or that the limit is higher than what Tetarenko et al (2016) thought. However, even though the most widely accepted distance of Swift J1745-26 is 7 kpc (Curran et al 2014;Kalemci et al 2014), this value is poorly constrained (Muñoz-Darias et al 2013). Thus, if we assume a distance lower than ∼4 kpc, even the BHT Swift J1745-26 would fall within the proposed upper limit of 0.11 L Edd .…”

Section: Discussionmentioning

confidence: 88%

The long outburst of the black hole transient GRS 1716–249 observed in the X-ray and radio band

Bassi

Santo

D’Aí

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present the spectral and timing analysis of X-ray observations performed on the Galactic black hole transient GRS 1716-249 during the 2016-2017 outburst. The source was almost continuously observed with the Neil Gehrels Swift Observatory from December 2016 until October 2017. The X-ray hardness ratio and timing evolution indicate that the source approached the soft state three times during the outburst, even though it never reached the canonical soft spectral state. Thus, GRS 1716-249 increases the number of black hole transients showing outbursts with "failed" state transition. During the softening events, XRT and BAT broadband spectral modeling, performed with thermal Comptonization plus a multicolor disc black-body, showed a photon index (Γ < 2) and an inner disc temperature (kT in = 0.2-0.5 keV) characteristic of the hard intermediate state. This is in agreement with the root mean square amplitude of the flux variability (rms > 10%). We find that, coherently with a scenario in which the disc moves closer to the compact object, the accretion disc inner radius decreases with the increase of the inner disc temperature, until a certain point when the temperature starts to increase at constant radius. This, in addition with the spectral analysis results, suggests that either the accretion disc reached the innermost stable circular orbit during the hard intermediate state or the hot accretion flow might re-condensate in an inner mini-disc. We report on the radio observations performed during the outburst finding that GRS 1716-249 is located on the radio-quiet "outlier" branch of the radio/X-ray luminosity plane.

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Section: Discussionmentioning

confidence: 88%

The long outburst of the black hole transient GRS 1716–249 observed in the X-ray and radio band

Bassi

Santo

D’Aí

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…from E to F On the return branch from soft to hard, as we have seen above the reverse track is followed, through the SIMS and the HIMS, on a time scale compa-rable to that of the upper track. Observations of several transitions from multiple systems have shown that the compact radio jet is re-formed not in correspondence to the SIMS-HIMS transition, but when the system has reached the LHS, a delay of several days (see [74,73] and references therein. At the time of radio re-appearance, secondary maxima have been seen in the optical-infrared band, which have been attributed to direct jet emission, although alternative models exist [74].…”

Section: Radio Jetsmentioning

confidence: 99%

Transient Black Hole Binaries

Belloni

Motta

2016

Astrophysics and Space Science Library

148

108

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The last two decades have seen a great improvement in our understand- ing of the complex phenomenology observed in transient black-hole binary systems, especially thanks to the activity of the Rossi X-Ray Timing Explorer satellite, com- plemented by observations from many other X-ray observatories and ground-based radio, optical and infrared facilities. Accretion alone cannot describe accurately the intricate behavior associated with black-hole transients and it is now clear that the role played by different kinds of (often massive) outflows seen at different phases of the outburst evolution of these systems is as fundamental as the one played by the accretion process itself. The spectral-timing states originally identified in the X-rays and fundamentally based on the observed effect of accretion, have acquired new importance as they now allow to describe within a coherent picture the phenomenology observed at other wave- length, where the effects of ejection processes are most evident. With a particular focus on the phenomenology seen in the X-ray band, we review the current state-of-the-art of our knowledge of black hole transients, describing the accretion-ejection connection at play during outbursts through the evolution of the observed spectral-timing properties. Although we mainly concentrate on the ob- servational aspects of the global X-ray transient picture, we also provide physical insight to it by reviewing (when available) the theoretical explanations and models proposed to explain the observed phenomenology.Comment: 37 pages, 7 figures, to be published in: "Astrophysics of Black Holes - From fundamental aspects to latest developments", Ed. Cosimo Bambi, Springer: Astrophysics and Space Science Library. arXiv admin note: text overlap with arXiv:0708.0148 by other author

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“…1. X-rays heating the companion, increasing the mass accretion rate (outburst 'echos'; see Lasota 2001;Dubus et al 2001;Kalemci et al 2014, and references therein), 2. synchrotron emission from the reactivation of the jet in the hard state decay (e.g. Kalemci et al 2013),…”

Section: Introductionmentioning

confidence: 99%

Bright Mini-outburst Ends the 12 yr Long Activity of the Black Hole Candidate Swift J1753.5–0127

Zhang

Bernardini

Russell

et al. 2019

ApJ

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We present optical, UV and X-ray monitoring of the short orbital period black hole X-ray binary candidate Swift J1753.5-0127, focusing on the final stages of its 12−year long outburst that started in 2005. From September 2016 onward, the source started to fade and within three months, the optical flux almost reached the quiescent level. Soon after that, using a new proposed rebrightening classification method we recorded a mini-outburst and a reflare in the optical light curves, peaking in February (V∼17.0) and May (V∼17.9) 2017, respectively. Remarkably, the mini-outburst has a peak flux consistent with the extrapolation of the slow decay before the fading phase preceding it. The following reflare was fainter and shorter. We found from optical colors that the temperature of the outer disk was ∼ 11,000 K when the source started to fade rapidly. According to the disk instability model, this is close to the critical temperature when a cooling wave is expected to form in the disk, shutting down the outburst. The optical color could be a useful tool to predict decay rates in some X-ray transients. We notice that all X-ray binaries that show mini-outbursts following a main outburst are short orbital period systems (< 7 h). In analogy with another class of short period binaries showing similar mini-outbursts, the cataclysmic variables of the RZ LMi type, we suggest mini-outbursts could occur if there is a hot inner disk at the end of the outburst decay.

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Multiwavelength observations of the black hole transient Swift J1745−26 during the outburst decay

Cited by 14 publications

References 61 publications

The long outburst of the black hole transient GRS 1716–249 observed in the X-ray and radio band

The long outburst of the black hole transient GRS 1716–249 observed in the X-ray and radio band

Transient Black Hole Binaries

Bright Mini-outburst Ends the 12 yr Long Activity of the Black Hole Candidate Swift J1753.5–0127

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