  We have analyzed archival Ginga data of a number of Soft X-ray Transient
sources and modelled them in an attempt to constrain the geometry and physical
properties of accretion. Our models include a self-consistent description of
X-ray reprocessing, linking the properties of the reflected continuum and those
of the iron fluorescence K\alpha line, and allowing for relativistic smearing
of spectral features. We derive constraints on the inner extent of the disk and
its ionization, assuming a generic geometry of a central X-ray source and an
external accretion disk.
  Fitting our models to the data we have found that in some sources - GS
1124-68 (Nova Muscae 1991) and GS 2000+25 - the evolution during decline
proceeded in qualitative agreement with recent theoretical models based on
advection-dominated solutions of accretion flow. These models link the
high/soft-low/hard transition with a change of geometry, most importantly, the
inner radius of the optically thick disk. Quantitatively, our analysis requires
serious revision of the model assumptions.
  A remarkably exceptional case is that of GS 2023+338, where the source
behavior both during outburst and decline was quite different than the other,
more ``standard'' ones. However, we found that the source did go into the
high/soft state, contrary to claims in literature.
