Echoes in X-ray Binaries
arXiv:astro-ph/0204018 · doi:10.1046/j.1365-8711.2002.05530.x
Abstract
We present a method of analysing the correlated X-ray and optical/UV variability in X-ray binaries, using the observed time delays between the X-ray driving lightcurves and their reprocessed optical echoes. This allows us to determine the distribution of reprocessing sites within the binary. We model the time-delay transfer functions by simulating the distribution of reprocessing regions, using geometrical and binary parameters. We construct best-fit time-delay transfer functions, showing the regions in the binary responsible for the reprocessing of X-rays. We have applied this model to observations of the Soft X-ray Transient, GRO j1655-40. We find the optical variability lags the X-ray variability with a mean time delay of 19.3 seconds. This means that the outer regions of the accretion disc are the dominant reprocessing site in this system. On fitting the data to a simple geometric model, we derive a best-fit disk half-opening angle of 13.5 degrees, which is similar to that observed after the previous outburst by cite{orosz97}. This disk thickening has the effect of almost entirely shielding the companion star from irradiation at this stage of the outburst.
accepted for publication in MNRAS
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