DURING OUTBURSTS BLACK HOLE (BH) TRANSIENTS ENTER INTO DIFFERENT SPECTRAL STATES DEPENDING ON THE MASS ACCRETION RATE AS WELL AS AT LEAST ONE OTHER PHYSICAL PARAMETER. ALTHOUGH WE DO NOT KNOW WHICH SECOND. PARAMETER IS MOST IMPORTANT CANDIDATES INCLUDE JET POWER DISK VISCOSITY (WHICH MAY BE RELATED TO MAGNETIC FIELD GENERATION AND TRANSPORT) AND INNER DISK RADIUS. THE RECURRENT (RV20 OUTBURSTS TO DATE) BH TRANSIENT 4U 1630-47 USUALLY EXHIBITS DIFFERENT STATE EVOLUTION THAN OTHER SYSTEMS. IN PARTICULAR DURING OUTBURST DECAY WE FOUND THAT ITS SPECTRUM CAN REMAIN SOFT DOWN TO VERY LOW LUMINOSITY AND THIS MAY INDICATE A LOW DISK VISCOSITY. WE PROPOSE AN XMM TOO TO CONSTRAIN THE ORIGIN OF THE LOW-SOFT STATE EMISSION WHICH HAS IMPLICATIONS FOR THE DISK GEOMETRY AND VISCOSITY.