The black hole candidate X-ray transient XTE J1817 - 330 was observed by the Swift satellite over 160 days of its 2006 outburst with the XRT and UVOT instruments .
At the start of the observations , the XRT spectra show that the 0.6-10 keV emission is dominated by an optically thick , geometrically thin accretion disk with an inner disk temperature of \sim 0.8 keV , indicating that the source was in a high/soft state during the initial outburst phase .
We tracked the source through its decline into the low/hard state with the accretion disk cooling to \sim 0.2 \mathrm { keV } and the inner disk radius consistent with the innermost stable circular orbit at all times .
Furthermore , the X-ray luminosity roughly follows L _ { X } \propto T ^ { 4 } during the decline , consistent with a geometrically stable blackbody .
These results are the strongest evidence yet obtained that accretion disks do not automatically recede after a state transition , down to accretion rates as low as 0.001 L _ { Edd } .
Meanwhile , the near-UV flux does not track the X-ray disk flux , and is well in excess of what is predicted if the near-UV emission is from viscous dissipation in the outer disk .
The strong correlation between the hard X-ray flux and the near-UV flux , which scale as L _ { X } ^ { 0.5 } , indicate that reprocessed emission is most likely the dominate contribution to the near-UV flux .
We discuss our results within the context of accretion disks and the overall accretion flow geometry in accreting black holes .