Re-analysis of some archival X–ray data of black hole binaries in soft spectral states is presented .
Results of detailed spectral fitting , including proper physical description of the X–ray reprocessed component , indicate that in most cases the soft , thermal disk emission can not be described by a simple multi-color blackbody model .
Additional Comptonization of those seed photons provides an acceptable description of the soft component , implying a presence of a warm ( kT _ { e } \sim 1 keV ) , mildly optically thick ( \tau \sim 10 ) phase of accreting plasma .

Combined spectral/temporal analysis of GS 1124-68 during ’ flip-flop ’ transitions in VHS suggests that the optically thick accretion flow can proceed in ( at least ) two modes giving the same time-integrated behaviour ( i.e .
energy spectra ) but very different timing behaviour .