On the X-ray time-lags in the black hole candidates

By O. Kotov, E. Churazov, M. Gilfanov. 2001

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Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/acf6a1efe44cd930afc859ac7593b212f66c8965

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Citations in the corpus

Broad iron L line and X-ray reverberation in 1H0707-495 (2009, background): “Several models have been suggested to explain the lag, the most successful of which is the propagation of accretion fluctuations (Lyubarskii 1997; Kotov et al. 2001, see also Arévalo & Uttley 2006).”
A physical model for the continuum variability and QPO in accreting black holes (2011, background): “This naturally produces a light curve which has an rms-flux relation/lognormal flux distribution (Kotov et al 2001: hereafter K01; Arevalo & Uttley 2006: hereafter AU06; also see Misra & Zdziarski 2008).”
Rapid optical and X-ray timing observations of GX 339-4: multi-component optical variability in the low/hard state (2010, background): “…to lower source fluxes by about a factor of 2 – we found a high coherence value of ≈0.9–1 over much of the Fourier frequency range, and a logarithmic time lag decline (within the errors) to high frequencies (e.g. Miyamoto et al. 1992; Vaughan & Nowak 1997; Nowak et al. 1999b; Kotov et al. 2001).”
Investigating a fluctuating-accretion model for the spectral-timing properties of accreting black hole systems (2005, methodology): “Besides explaining the broad range of variability timescales and the rms-flux relation, the fluctuating accretion model can also explain the spectral-timing properties of the variability, as noted by Kotov et al. (2001).”
X-ray continuum variability of MCG-6-30-15 (2002, methodology): “A simple phenomenological model has been developed by Lyubarskii (1997), Churazov et al. (2001), and Kotov et al. (2001) that seems to explain (qualitatively, at least) the temporal properties of Cyg X-1.”
Relativistic iron K X-ray reverberation in NGC 4151 (2011, background): “A distant reflector with a narrow line at 6.4 keV and an edge at 7.1 keV can possibly produce a broad line-like structure similar to that seen here (e.g. Kotov et al. 2001 for black hole binaries modelling).”
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).”
A global look at X-ray time lags in seyfert galaxies (2016, background): “Kotov et al. (2001) and later Arévalo & Uttley (2006) extended this idea further to explain the time lags in the X-ray emission.”
Combined long and short timescale X-ray variability of NGC 4051 with RXTE and XMM-Newton (2003, background): “Recently Churazov et al. (2001), with later enhancements by Kotov et al. (2001), have built a qualitative geometric model which can explain many of the observational results presented here (cf Vaughan et al. 2003).”
Active galactic nuclei: what’s in a name? (2017, background): “However, if due to the slower, viscous propagation in the flow the large lags can be easily recovered in standard disk-corona geometries (e.g. Kotov et al. 2001; Arévalo and Uttley 2006).”
X-ray reverberation around accreting black holes (2014, background): “As noted however, reverberation cannot explain the large hard lags observed at low frequencies (Kotov et al. 2001; Cassatella et al. 2012b).”