Superhump period of the black hole X-ray binary GX 339−4

Kosenkov, Ilia A.; Veledina, Alexandra

doi:10.1093/mnras/sty1142

Cited by 11 publications

(10 citation statements)

References 33 publications

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“…5b; also ). In about 40 d (MJD 52440), when the flux started to decrease, the variability, which was previously attributed to superhumps (Kosenkov & Veledina 2018), became apparent. At the time of this change, the ASM fluxes and ASM B/A hardness ratio had a local minimum (see Fig.…”

Section: Regular Outburstsmentioning

confidence: 74%

“…The SS contour is elongated along the blackbody track, but there is some spread of the data points around the model. This is likely caused by the variability due to superhumps (Kosenkov & Veledina 2018).…”

Section: Outburst Templatementioning

confidence: 99%

“…where µ j is the slope, which can be positive or negative. In this equation, m j is the observed magnitude in jth ONIR filter, m 0 j is the constant, t is the time, t 0 is either the beginning (if the fitted data set covers the first part of the SS) or the end time of the fitted data set (if it covers the last part of the SS), and j is the intrinsic scatter, which is partially caused by superhump variability (Dinçer et al 2012;Kosenkov & Veledina 2018). We use Bayesian inference to estimate these parameters and list these in Table 5.…”

Section: Evolution Of the Nonthermal Componentmentioning

confidence: 99%

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Colors and patterns of black hole X-ray binary GX 339-4

Kosenkov

Veledina

Suleimanov

et al. 2020

A&A

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Black hole X-ray binaries show signs of nonthermal emission in the optical to near-infrared range. We analyzed optical to near-infrared SMARTS data on GX 339-4 over the 2002–2011 period. Using soft state data, we estimated the interstellar extinction toward the source and characteristic color temperatures of the accretion disk. We show that various spectral states of regular outbursts occupy similar regions on color-magnitude diagrams, and that transitions between the states proceed along the same tracks despite substantial differences in the morphology of the observed light curves. We determine the typical duration of hard-to-soft and soft-to-hard state transitions and the hard state at the decaying stage of the outburst to be one, two, and four weeks, respectively. We find that the failed outbursts cannot be easily distinguished from the regular outbursts at their early stages, but if the source reaches 16 mag in V band, it transits to the soft state. By subtracting the contribution of the accretion disk, we obtain spectra of the nonthermal component, which have constant, nearly flat shapes during the transitions between the hard and soft states. In contrast to the slowly evolving nonthermal component seen at optical and near-infrared wavelengths, the mid-infrared spectrum is strongly variable on short timescales and sometimes shows a prominent excess with a cutoff below 1014 Hz. We show that the radio to optical spectrum can be modeled using three components corresponding to the jet, hot flow, and irradiated accretion disk.

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Section: Regular Outburstsmentioning

confidence: 74%

Section: Outburst Templatementioning

confidence: 99%

Section: Evolution Of the Nonthermal Componentmentioning

confidence: 99%

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Colors and patterns of black hole X-ray binary GX 339-4

Kosenkov

Veledina

Suleimanov

et al. 2020

A&A

Self Cite

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“…In particular, we find that the scenario where optical emission originates from the jet base and the IR emission originates from the particle acceleration region 𝑧 diss is consistent with the data. An alternative scenario is that both the IR and the optical emission originate in a hot flow that consists of thermal and non-thermal electrons (Poutanen & Veledina 2014;Kosenkov et al 2020), a scenario that better describes the soft states (Kosenkov & Veledina 2018). Further simultaneous IR-to-optical observations in the hard state would be able to test this scenario, as well as simultaneous polarisation measurements across the entire optical/IR band (although see e.g., Russell & Fender 2008 for measurements prior to the 2010 outburst).…”

Section: Multi-wavelength Spectrum and Jet Dynamicsmentioning

confidence: 99%

The prototype X-ray binary GX 339-4: using TeV gamma-rays to assess LMXBs as Galactic cosmic ray accelerators

Kantzas,

Markoff,

Lucchini

et al. 2022

Preprint

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Since the discovery of cosmic rays (CRs) over a century ago, their origin remains an open question. Galactic CRs with energy up to the knee (10 15 eV) are considered to originate from supernova remnants, but this scenario has recently been questioned due to lack of TeV 𝛾-ray counterparts in many cases. Extragalactic CRs on the other hand, are thought to be associated with accelerated particles in the relativistic jets launched by supermassive accreting black holes at the center of galaxies. Scaled down versions of such jets have been detected in X-ray binaries hosting a stellar black hole (BHXBs). In this work, we investigate the possibility that the smaller-scale jets in transient outbursts of low-mass BHXBs could be sources of Galactic CRs. To better test this scenario, we model the entire electromagnetic spectrum of such sources focusing on the potential TeV regime, using the 'canonical' low-mass BHXB GX 339-4as a benchmark. Taking into account both the leptonic radiative processes and the 𝛾-rays produced via neutral pion decay from inelastic hadronic interactions, we predict the GeV and TeV 𝛾-ray spectrum of GX 339-4 using lower-frequency emission as constraints. Based on this test-case of GX 339-4 we investigate whether other, nearby low-mass BHXBs could be detected by the next-generation very-high-energy 𝛾-ray facility the Cherenkov Telescope Array, which would establish them as additional and numerous potential sources of CRs in the Galaxy.

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“…As detailed in Section 2.3 of Paper I, eccentric distortions excited at a 3:1 resonance with the orbit of the X-ray binary (e.g., Lubow 1991) can very reasonably be expected to propagate all the way to the inner disc, especially in the presence of elevated accretion rates associated with the SPL state (see fig. 5 1996;Neil et al 2007;Zurita et al 2008;Kosenkov & Veledina 2018) indicate that black hole accretion discs in many of the systems are likely to be eccentric, although actual eccentricities are difficult to estimate, and to our knowledge there have been no direct measurements.…”

Section: Trapped R-mode Excitation and Hfqposmentioning

confidence: 99%

HFQPOs and discoseismic mode excitation in eccentric, relativistic discs. II. Magnetohydrodynamic simulations

Dewberry,

Latter,

Ogilvie

et al. 2020

Preprint

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Trapped inertial oscillations (r-modes) provide a promising explanation for high-frequency quasi-periodic oscillations (HFQPOs) observed in the emission from black hole X-ray binary systems. An eccentricity (or warp) can excite r-modes to large amplitudes, but concurrently the oscillations are likely damped by magnetohydrodynamic (MHD) turbulence driven by the magnetorotational instability (MRI). We force eccentricity in global, unstratified, zero-net flux MHD simulations of relativistic accretion discs, and find that a sufficiently strong disc distortion generates trapped inertial waves despite this damping. In our simulations, eccentricities above ∼ 0.03 in the inner disc excite trapped waves. In addition to the competition between r-mode damping and driving, we observe that larger amplitude eccentric structures modify and in some cases suppress MRI turbulence. Given the variety of distortions (warps as well as eccentricities) capable of amplifying r-modes, the robustness of trapped inertial wave excitation in the face of MRI turbulence in our simulations provides support for a discoseismic explanation for HFQPOs.

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Superhump period of the black hole X-ray binary GX 339−4

Cited by 11 publications

References 33 publications

Colors and patterns of black hole X-ray binary GX 339-4

Colors and patterns of black hole X-ray binary GX 339-4

The prototype X-ray binary GX 339-4: using TeV gamma-rays to assess LMXBs as Galactic cosmic ray accelerators

HFQPOs and discoseismic mode excitation in eccentric, relativistic discs. II. Magnetohydrodynamic simulations

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