Accretion and outflow in V404 Cyg

Casares, J.; Muñoz-Darias, T.; Sánchez, D. Mata; Charles, P. A.; Torres, M. A. P.; Padilla, M. Armas; Fender, R. P.; García‐Rojas, J.

doi:10.1093/mnras/stz1793

Cited by 30 publications

(29 citation statements)

References 109 publications

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“…He i λ5876 is found to show persistent P-Cygni profiles in the spectra of MAXI J1820+070 taken during the Xray low/hard state, as similarly reported by Muñoz-Darias et al (2019). Similar P-Cygni profile was also seen in V404 Cygni and other BH LMXBs (Mata Sánchez et al 2018;Casares et al 2019), where the continuous presence of P-Cygni profiles were proposed to result from an expanding outflow formed during the outburst. One can notice that there is a prominent absorption feature on the red side of He i λ5876, which is likely due to the Galactic Na i D absorption doublet.…”

Section: He I λ5876 Featuresupporting

confidence: 81%

Optical and Ultraviolet Monitoring of the Black Hole X-ray Binary MAXI J1820+070/ASASSN-18ey for 18 Months

Sai,

Wang,

et al. 2021

Preprint

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MAXI J1820+070 is a low-mass black hole X-ray binary system with high luminosity in both optical and X-ray bands during the outburst periods. We present extensive photometry in X-ray, ultraviolet, and optical bands, as well as densely-cadenced optical spectra, covering the phase from the beginning of optical outburst to ∼550 days. During the rebrightening process, the optical emission preceded the X-ray by 20.80 ± 2.85 days. The spectra are characterized by blue continua and emission features of Balmer series, He i, He ii lines and broad Bowen blend. The pseudo equivalent width (pEW) of emission lines are found to show anticorrelations with the X-ray flux measured at comparable phases, which is due to the increased suppression by the optical continuum. At around the X-ray peak, the full width at half maximums (FWHMs) of H β and He ii λ4686 tend to stabilize at 19.4 Angstrom and 21.8 Angstrom, which corresponds to the line forming region at a radius of 1.7 and 1.3 R within the disk. We further analyzed the absolute fluxes of the lines and found that the fluxes of H β and He ii λ4686 show positive correlations with the X-ray flux, favoring that the irradiation model is responsible for the optical emission. However, the fact that X-ray emission experiences a dramatic flux drop at t∼200 days after the outburst, while the optical flux only shows little variations suggests that additional energy such as viscous energy may contribute to the optical radiation in addition to the X-ray irradiation.

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Section: He I λ5876 Featuresupporting

confidence: 81%

Optical and Ultraviolet Monitoring of the Black Hole X-ray Binary MAXI J1820+070/ASASSN-18ey for 18 Months

Sai,

Wang,

et al. 2021

Preprint

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“…These two objects display non-standard outbursts characterised by sharp rising phases followed by significant luminosity drops and the absence of steady soft states (e.g. Casares et al 2019 for V404 Cyg). The discovery outburst of Swift J1858.6-0814 is still ongoing and it is beyond the scope of this paper to discuss the outburst evolution.…”

Section: Discussionmentioning

confidence: 99%

The Changing-look Optical Wind of the Flaring X-Ray Transient Swift J1858.6-0814

Muñoz-Darias

Padilla

Jiménez-Ibarra

et al. 2020

ApJL

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We present the discovery of an optical accretion disk wind in the X-ray transient Swift J1858.6-0814. Our 90-spectrum data set, taken with the 10.4m GTC telescope over 8 different epochs and across five months, reveals the presence of conspicuous P-Cyg profiles in He i at 5876Å and Hα. These features are detected throughout the entire campaign, albeit their intensity and main observational properties are observed to vary on time-scales as short as five minutes. In particular, we observe significant variations in the wind velocity, between a few hundreds and ∼ 2400 km s −1 . In agreement with previous reports, our observations are characterised by the presence of frequent flares, although the relation between the continuum flux variability and the presence/absence of wind features is not evident. The reported high activity of the system at radio waves indicates that the optical wind of Swift J1858.6-0814 is contemporaneous with the radio-jet, as is the case for the handful of X-ray binary transients that have shown so far optical P-Cyg profiles. Finally, we compare our results with those of other sources showing optical accretion disk winds, with emphasis on V404 Cyg and V4641 Sgr, since they also display strong and variable optical wind features as well as similar flaring behaviour.

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“…Accretion disc winds are arguably the last relevant ingredient added to the LMXB accretion picture, since there is increasing evidence suggesting that they carry away a significant fraction of the mass involved in the accretion process (e.g. Neilsen et al 2011;Ponti et al 2012;Muñoz-Darias et al 2016;Casares et al 2019) as well as angular momentum (e.g. Tetarenko et al 2018;Dubus et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Near-infrared emission lines trace the state-independent accretion disc wind of the black hole transient MAXI J1820+070

Sánchez-Sierras

Muñoz-Darias

2020

A&A

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The black hole transient MAXI J1820+070 displayed optical P Cyg profiles and other wind-related emission line features during the hard state of its discovery outburst. We present near-infrared (NIR) spectroscopy covering the different accretion states of the system during this event. Our eight-epoch data set (VLT/X-shooter) reveals strong variability in the properties of the NIR emission lines. This includes absorption troughs and extended emission line wings with kinetic properties that are remarkably similar to those inferred from the wind signatures observed in optical emission lines, indicating that they most likely trace the same accretion disc wind. Unlike the optical features, these NIR signatures are not exclusive of the hard state, as they are also witnessed across the soft state with similar observational properties. This supports the presence of a relatively steady outflow during the entire outburst of the system, and it represents the first detection of an accretion disc wind in a black hole soft state at energies other than X-rays. We discuss the visibility of the wind as a function of the spectral band and the potential of NIR spectroscopy for wind studies, in particular during luminous accretion phases.

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Accretion and outflow in V404 Cyg

Cited by 30 publications

References 109 publications

Optical and Ultraviolet Monitoring of the Black Hole X-ray Binary MAXI J1820+070/ASASSN-18ey for 18 Months

Optical and Ultraviolet Monitoring of the Black Hole X-ray Binary MAXI J1820+070/ASASSN-18ey for 18 Months

The Changing-look Optical Wind of the Flaring X-Ray Transient Swift J1858.6-0814

Near-infrared emission lines trace the state-independent accretion disc wind of the black hole transient MAXI J1820+070

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