Infrared photometry of the dwarf nova V2051 Ophiuchi – II. The quiescent accretion disc and its spiral arms

Baptista, R.; Wojcikiewicz, Eduardo

doi:10.1093/mnras/stz3517

Cited by 5 publications

(3 citation statements)

References 52 publications

(89 reference statements)

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“…Other LMXBs are known to exhibit quiescent flickering, but the magnitude of quiescent variability of GX 339-4 and significant changes in observed colors exceed that measured for other sources (Zurita et al 2003). A possible explanation for this behavior is the emission from the spiral arms, hotspots, and hot line flares triggered by the magnetic field reconnection in the vicinity of the disk, and the presence of edges and lines in the quiescent spectra (see, e.g., Zurita et al 2003;Cherepashchuk et al 2019;Baptista & Wojcikiewicz 2020).…”

Section: Onir Spectramentioning

confidence: 97%

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: Onir Spectramentioning

confidence: 97%

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

Kosenkov

Veledina

Suleimanov

et al. 2020

A&A

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“…The spiral shock is easily produced due to the disk instabilities or tidal perturbations in the non-axisymmetric flow, even in the inviscid flow, which has been confirmed by various simulation studies (Sawada et al 1986a,b;Savonije et al 1994;Rafikov 2002;Bisikalo et al 2004;Kurbatov et al 2014;Arzamasskiy & Rafikov 2018). Simultaneously, observations also confirm the presence of spiral structure and spiral shock in the accretion disk (Steeghs et al 1997;Neustroev & Borisov 1998;Pala et al 2019;Baptista & Wojcikiewicz 2020;Lee et al 2020).…”

Section: Introductionmentioning

confidence: 61%

Point-wise Self-similar Solution for Spiral Shocks in Accretion Disk with Mass Outflow in Binary

Aktar,

Xue,

Liu

2021

Preprint

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We examine the properties of spiral shocks from a steady, adiabatic, non-axisymmetric accretion disk around a compact star in binary. We first time incorporate all the possible influences from binary through adopting the Roche potential and Coriolis forces in the basic conservation equations. In this paper, we assume the spiral shocks to be point-wise self-similar, and the flow is in vertical hydrostatic equilibrium to simplify the study. We also investigate the mass outflow due to the shock compression and apply it to the accreting white dwarf in binary. We find that our model will be beneficial to overcome the ad hoc assumption of optically thick wind generally used in the studies of the progenitor of supernovae Ia.

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“…The existence of spiral structures in accretion disks has long been a topic of interest in both observational and theoretical studies. Observations have provided many pieces of evidence for the existence of a spiral structure in accretion disks (Steeghs et al 1997;Neustroev & Borisov 1998;Pala et al 2019;Baptista & Wojcikiewicz 2020;Lee et al 2020), and there is a general consensus that the spiral shock wave induces a spiral structure in the accretion disk. However, the origin of the shock may correspond to many different mechanisms.…”

Section: Introductionmentioning

confidence: 99%

Spiral shocks induced in a galactic gaseous disk: Hydrodynamic understanding of observational properties of spiral galaxies

Aktar,

Xue,

Zhang

et al. 2023

A&A

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Context. We investigate the properties of spiral shocks in a steady, adiabatic, non-axisymmetric, self-gravitating, mass-outflowing accretion disk around a compact object. Aims. We obtained the accretion-ejection solutions in a galactic disk and applied them to spiral galaxies in order to investigate the possible physical connections between some observational quantities of galaxies. Methods. We considered the self-gravitating disk potential to examine the properties of the galactic gaseous disk. We obtained spiral shock-induced accretion-ejection solutions following the point-wise self-similar approach. Results. We observed that the self-gravitating disk profoundly affects the dynamics of the spiral structure of the disk and the properties of the spiral shocks. We find that the observational dispersion between the pitch angle and shear rate and between the pitch angle and star formation rate in spiral galaxies contains some important physical information. Conclusions. There are large differences among the star formation rates of galaxies with similar pitch angles. These differences may be explained by the different star formation efficiencies caused by distinct galactic ambient conditions.

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Infrared photometry of the dwarf nova V2051 Ophiuchi – II. The quiescent accretion disc and its spiral arms

Cited by 5 publications

References 52 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

Point-wise Self-similar Solution for Spiral Shocks in Accretion Disk with Mass Outflow in Binary

Spiral shocks induced in a galactic gaseous disk: Hydrodynamic understanding of observational properties of spiral galaxies

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