A disc-corona radiative feedback loop with a time delay produces QPOs at 1/(tau_A+tau_B), and its analytic power spectrum fits AstroSat data of two black hole binaries.
A Compton Up-scattering Model for Soft Lags in the Lower Kilohertz QPO in 4U1608-52
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abstract
An empirical Compton up-scattering model is described which reproduces both the fractional amplitude (RMS) vs. energy and the soft time lags in the 830 Hz QPO observed in 4U1608-52 on Mar. 3, 1996. A combination of two coherent variations in the coronal and soft photon temperatures (with their relative contributions determined by enforcing energy conservation) gives rise to the QPO's energy dependent characteristics. All input parameters to the model, save a characteristic plasma size and the fraction of Comptonized photons impinging on the soft photon source, are derived from the time-averaged photon energy spectrum of the same observation. Fits to the fractional RMS and phase lag data for this kilohertz QPO imply that the spatial extent of the plasma is in the range from 4 to 15 km.
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Quasi-Periodic Oscillations due to radiative feedback mechanism between the disc and corona
A disc-corona radiative feedback loop with a time delay produces QPOs at 1/(tau_A+tau_B), and its analytic power spectrum fits AstroSat data of two black hole binaries.