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We report on the geometry of accretion disk and high energy coronae in thestrong Comptonization state (the very high/steep power law/hard intermediatestate) based on a Suzaku observation of the famous Galactic black hole GX339-4. 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 be2.9E38 erg/s for a distance of 8 kpc. We fit the spectrum with both simple(independent disk and corona) and sophisticated (energetically coupled disk andcorona) models, but all fits imply that the underlying optically thick disk istruncated significantly before the innermost stable circular orbit around theblack hole. We show this directly by a comparison with similarly broadband datafrom a disk dominated spectrum at almost the same luminosity observed byXMM-Newton and RXTE 3 days after the Suzaku observation.  During the Suzaku observation, the QPO frequency changes from 4.3 Hz to 5.5Hz, while the spectrum softens. The energetically coupled model gives acorresponding 5+/- 8 % decrease in derived inner radius of the disk. While thisis not significant, it is consistent with the predicted change in QPO frequencyfrom Lense-Thirring precession of the hot flow interior to the disk and/or adeformation mode of this flow, as a higher QPO frequency implies a smaller sizescale for the corona. This is consistent with the truncated disk extendingfurther inwards towards the black hole.

The truncated disk from Suzaku data of GX 339-4 in the extreme very high state