Soft state of Cygnus X‐1: stable disc and unstable corona

By E. Churazov, M. Gilfanov, M. Revnivtsev. 2001

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Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c768ba35719134e09fbab9c5b420b65017fa1de1

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Combined long and short timescale X-ray variability of NGC 4051 with RXTE and XMM-Newton (2003, background): “For GBHs, the PSDs of the high (eg Cui et al. 1997b, Churazov et al. 2001) and low (eg Nowak et al. 1999; Revnivtsev, Gilfanov and Churazov 2000) states are different, thereby providing us with a means of discrimination.”
Investigating a fluctuating-accretion model for the spectral-timing properties of accreting black hole systems (2005, background): “However, the fluctuations need not only be produced but also propagated, which poses a difficulty for much thinner accretion flows, as fluctuations on time-scales much shorter than the propagation time-scale are easily damped (Churazov et al. 2001).”
MODELING THE TIME VARIABILITY OF SDSS STRIPE 82 QUASARS AS A DAMPED RANDOM WALK (2010, background): “Moreover, these fluctuations in the fueling rate will also be smoothed out and damped as they travel inward, and will likely have effectively disappeared by the time they reach the optical emitting region (e.g., see discussion in Churazov et al. 2001).”
Correlations between X-ray and radio spectral properties of accreting black holes (2002, background): “F anticorrelation) is seen in the soft state of Cyg X-1 (Churazov, Gilfanov & Revnivtsev 2001; Z02), in which case coronal models are widely accepted (e.g. Poutanen et al. 1997; Gierliński et al. 1999; Churazov et al. 2001).”
Long term variability of Cygnus X-1. I. X-ray spectral-temporal correlations in the hard state (2002, background): “…there exists no consistent model for explaining the complex short term variability on time scales faster than 1000 s, although several phenomenological models have been discussed (Böttcher 2001; Kotov et al. 2001; Poutanen 2002; Churazov et al. 2001; Nowak et al. 2002; Kazanas et al. 1997).”
Accretion disc variability in the hard state of black hole X-ray binaries (2009, background): “Alternatively, the optically thick and optically thin components may co-exist ⋆ E-mail: t.r.wilkinson@phys.soton.ac.uk over some range of radii, e.g. if the thin disc is sandwiched by a hot flow or corona (Witt, Czerny & Zycki 1997; Churazov et al. 2001).”
Low-frequency oscillations in black holes: a spectral-timing approach to the case of GX 339-4 (2011, background): “Since LFQPOs are known to be usually associated to the hard tail of the spectrum (see Churazov et al. 2001 and Sobolewska &Życki 2006, but also Rodriguez et al. 2004 and Rodriguez et al. 2008, who showed tha LFQPO spectra display a moving high energy cutoff), we started investigating the relations…”
A physical model for the continuum variability and QPO in accreting black holes (2011, background): “The low frequency break is close to the frequency of the viscous timescale atro, as proposed by e.g. by Churazov et al (2001); Gilfanov & Areief (2005); DGK07; Ingram & Done (2010).”
X-ray continuum variability of MCG-6-30-15 (2002, methodology): “…break in the PSD fromf−1 to a steeper slope (as seen in MCG–6-30-15) is due to suppressionof fluctuations within the X-ray emitting region, and the timescale of the break in the PSD corresponds to the characteristic timescale at the outer radius of the X-ray emitting region (Churazov et al. 2001).”
On the X-ray time-lags in the black hole candidates (2001, background): “However due to suppression of the high frequency variations in the course of diffusion such situation may in practice materialize in the accretion flow if the times scales of locally induced perturbations at given radius are high, e.g. higher than the diffusion frequency (Churazov et al. 2001).”
Modelling the behaviour of accretion flows in X-ray binaries (2007, background): “This acts as a low pass filter, suppressing any faster fluctuations in the mass accretion rate through the disc due to the inability of the disc to respond to these (Psaltis & Norman 2000, Churazov et al. 2001).”
Active galactic nuclei: what’s in a name? (2017, background): “…of the perturbations is longer than the radial diffusion time, the perturbations can propagate inward, combining multiplicatively with perturbations produced at smaller radii, and reach the innermost zones where most of the energy is released (e.g. Churazov et al. 2001; Hogg and Reynolds 2016).”