  We report on the geometry of accretion disk and high energy coronae in the
strong Comptonization state (the very high/steep power law/hard intermediate
state) based on a Suzaku observation of the famous Galactic black hole GX
339-4. These data were taken just before the peak of the 2006-2007 outburst,
and the average X-ray luminosity in the 0.7-200 keV band is estimated to be
2.9E38 erg/s for a distance of 8 kpc. We fit the spectrum with both simple
(independent disk and corona) and sophisticated (energetically coupled disk and
corona) models, but all fits imply that the underlying optically thick disk is
truncated significantly before the innermost stable circular orbit around the
black hole. We show this directly by a comparison with similarly broadband data
from a disk dominated spectrum at almost the same luminosity observed by
XMM-Newton and RXTE 3 days after the Suzaku observation.
  During the Suzaku observation, the QPO frequency changes from 4.3 Hz to 5.5
Hz, while the spectrum softens. The energetically coupled model gives a
corresponding 5+/- 8 % decrease in derived inner radius of the disk. While this
is not significant, it is consistent with the predicted change in QPO frequency
from Lense-Thirring precession of the hot flow interior to the disk and/or a
deformation mode of this flow, as a higher QPO frequency implies a smaller size
scale for the corona. This is consistent with the truncated disk extending
further inwards towards the black hole.
