Second outburst of the black hole candidate MAXI J1836-194 from SWIFT and INTEGRAL observations

Гребенев, С. А.; Prosvetov, A. V.; Sunyaev, R.

doi:10.1134/s1063773713060054

Cited by 9 publications

(7 citation statements)

References 18 publications

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“…Note the short (∼ 10 days) dip by ∼ 40 − 50% in the 2-4 keV light curve observed shortly after maximum light. A similar dip was observed previously in the light curve of another X-ray nova, MAXI J1836-194 (Grebenev et al 2013), and was explained by the transition of the source to a harder spectral state in the standard X-ray band, which is probably associated with the disappearance of the soft blackbody spectral component (or a noticeable decrease in its temperature).…”

Section: Resultssupporting

confidence: 85%

“…It is generally believed that such an emission appears in low-mass X-ray binaries due to the irradiation and heating of the outer cold accretion disk by X-ray photons from its hot central zone (Lyuty and Sunyaev 1976). However, recent studies of the broadband spectra for several X-ray novae, XTE J1118+480 (Chaty et al 2003), MAXI J1836-194 (Grebenev et al 2013), and SWIFT J174510.8-26241 (Grebenev et al 2014), in their hard spectral state have shown that the OIR and UV emissions from these sources are an extension of the power law observed in the X-ray band and contain no clear evidence of a thermal emission component from the outer disk regions (see also Poutanen and Veledina 2014). Observations of the X-ray nova MAXI J1828-249 can give additional information for investigating this question.…”

Section: Introductionmentioning

confidence: 99%

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X-ray nova MAXI J1828-249. Evolution of the broadband spectrum during its 2013–2014 outburst

et al. 2016

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Based on data from the SWIFT, INTEGRAL, MAXI/ISS orbital observatories, and the ground-based RTT-150 telescope, we have investigated the broadband (from the optical to the hard X-ray bands) spectrum of the X-ray nova MAXI J1828-249 and its evolution during the outburst of the source in 2013-2014. The optical and infrared emissions from the nova are shown to be largely determined by the extension of the power-law component responsible for the hard X-ray emission. The contribution from the outer cold regions of the accretion disk, even if the X-ray heating of its surface is taken into account, turns out to be moderate during the source's "high" state (when a soft blackbody emission component is observed in the X-ray spectrum) and is virtually absent during its "low" ("hard") state. This result suggests that much of the optical and infrared emissions from such systems originates in the same region of main energy release where their hard X-ray emission is formed. This can be the Compton or synchro-Compton radiation from a high-temperature plasma in the central accretion disk region puffed up by instabilities, the synchrotron radiation from a hot corona above the disk, or the synchrotron radiation from its relativistic jets.

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Section: Resultssupporting

confidence: 85%

Section: Introductionmentioning

confidence: 99%

X-ray nova MAXI J1828-249. Evolution of the broadband spectrum during its 2013–2014 outburst

et al. 2016

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“…The outburst 'failed' to enter the full soft state, remaining in the HIMS (see Brocksopp et al 2004 for further discussion on failed outbursts), reaching its softest point on September 16, following which it transitioned back to the hard state on September 28 and faded towards quiescence. In 2012 March, the system underwent a period of renewed activity (Krimm et al 2012;Yang et al 2012;Grebenev et al 2013) before returning to quiescence by 2012 July 05 (Yang et al 2012b). This low-inclination system (between 4 • and 15 • ; Russell et al 2014b) is between 4 and 10 kpc away (Russell et al 2014a) and has proven itself to be an ideal system in which to study the evolution of the radio jet due to its bright radio emission (Russell et al 2013b;Russell et al 2014a).…”

Section: Introductionmentioning

confidence: 99%

Radio monitoring of the hard state jets in the 2011 outburst of MAXI J1836−194

Russell

Miller-Jones

Curran

et al. 2015

Monthly Notices of the Royal Astronomical Society

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MAXI J1836−194 is a Galactic black hole candidate X-ray binary that was discovered in 2011 when it went into outburst. In this paper, we present the full radio monitoring of this system during its 'failed' outburst, in which the source did not complete a full set of state changes, only transitioning as far as the hard intermediate state. Observations with the Karl G. Jansky Very Large Array (VLA) and Australia Telescope Compact Array (ATCA) show that the jet properties changed significantly during the outburst. The VLA observations detected linearly polarised emission at a level of ∼1% early in the outburst, increasing to ∼3% as the outburst peaked. High-resolution images with the Very Long Baseline Array (VLBA) show a ∼15 mas jet along the position angle −21 ± 2 • , in agreement with the electric vector position angle found from our polarisation results (−21 ± 4 • ), implying that the magnetic field is perpendicular to the jet. Astrometric observations suggest that the system required an asymmetric natal kick to explain its observed space velocity. Comparing quasi-simultaneous X-ray monitoring with the 5 GHz VLA observations from the 2011 outburst shows an unusually steep hard-state radio/X-ray correlation of L R ∝ L 1.8±0.2 X , where L R and L X denote the radio and X-ray luminosities, respectively. With ATCA and Swift monitoring of the source during a period of re-brightening in 2012, we show that the system lay on the same steep correlation. Due to the low inclination of this system, we then investigate the possibility that the observed correlation may have been steepened by variable Doppler boosting.

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“…Although significantly weaker than the first, it was followed by Swift and INTEGRAL. The resulting spectrum was consistent with a LHS, with no clear evidence of the presence of a soft component due to the accretion disc [153]. MAXI J1836−194 has been the subject of many studies since these initial observations, [438,437,436,197,374,196,108,259], but all were based on the data collected during the powerful first outburst, which demonstrates the importance of the role played by the wide field of view highenergy instruments like INTEGRAL.…”

Section: Maxi J1828−249mentioning

confidence: 72%

The INTEGRAL view on Black Hole X-ray Binaries

Motta,

Rodriguez,

Jourdain

et al. 2021

Preprint

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INTEGRAL is an ESA mission in fundamental astrophysics that was launched in October 2002. It has been in orbit for over 18 years, during which it has been observing the high-energy sky with a set of instruments specifically designed to probe the emission from hard X-ray and soft γ-ray sources. This paper is devoted to the subject of black hole binaries, which are among the most important sources that populate the high-energy sky. We present a review of the scientific literature based on INTEGRAL data, which has significantly advanced our knowledge in the field of relativistic astrophysics. We briefly summarise the state-of-the-art of the study of black hole binaries, with a particular focus on the topics closer to the INTEGRAL science. We then give an overview of the results obtained by INTEGRAL and by other observatories on a number of sources of importance in the field. Finally, we review the main results obtained over the past 18 years on all the black hole binaries that INTEGRAL has observed. We conclude with a summary of the main contributions of INTEGRAL to the field, and on the future perspectives.

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Second outburst of the black hole candidate MAXI J1836-194 from SWIFT and INTEGRAL observations

Cited by 9 publications

References 18 publications

X-ray nova MAXI J1828-249. Evolution of the broadband spectrum during its 2013–2014 outburst

X-ray nova MAXI J1828-249. Evolution of the broadband spectrum during its 2013–2014 outburst

Radio monitoring of the hard state jets in the 2011 outburst of MAXI J1836−194

The INTEGRAL view on Black Hole X-ray Binaries

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