  We identify the reflected component in the GINGA spectra of Nova Muscae, a
Black Hole transient system which has been used as the prototype for the recent
advection dominated disk models. We see that the reflected spectrum is
generally significantly relativistically smeared, and use this and the amount
of reflection to track the innermost extent of the accretion disk. We see that
the optically thick disk does retreat during the decline, but more slowly than
predicted by the advective models, posing problems for this description of the
accretion flow.
