MODELING THE TIME VARlABILITY OF ACCRETING COMPACT SOURCES

摘要

We present model light curves for accreting black hole candidates (BHCs) based on a recently pro- posed model for their spectro-temporal properties. According to this model, the observed light curves and aperiodic variabillty of BHCs are due to a series of soft photon injections at random (Poisson) inter- vals near the compact object and their reprocessing into hard radiation in an extended but nonuniform hot plasma corona surrounding the compact object. We argue that the majority of the timing character- istics of these light curves are due to the stochastic nature of the Comptonisation process in the extended corona, whose properties, most notably its radial density dependence, are imprinted in them. We compute the corresponding power spectral densities (PSD), autocorrelation functions, time skewness of the light curves, and time lags between the light curves of the sources at different photon energies and compare our results to observation. Our model light curves compare well with observations, providing good fits to their overall morphology, as manifest by the autocorrelation and skewness functions. The lags and PSDs of the model light curves are also in good agreement with those observed (the model can even accommodate the presence of quasi-Periodic oscilations). Finally, while most of the variability power resides at timescales approximately a few seconds, at the same time, the mode1 allows also for shots of a few milliseconds in duration, in accordance with observation. We suggest that refinements of this type of model along with spectral and phase lag information ca