  Context: The structure of the inner disk of Herbig Be stars is not well
understood. The continuum disks of several Herbig Be stars have inner radii
that are smaller than predicted by models of irradiated disks with optically
thin holes.
  Aims: We study the size of the inner disk of the Herbig B[e] star HD 85567
and compare the model radii with the radius suggested by the size-luminosity
relation.
  Methods: The object was observed with the AMBER instrument of the Very Large
Telescope Interferometer. We obtained K-band visibilities and closure phases.
These measurements are interpreted with geometric models and
temperature-gradient models.
  Results: Using several types of geometric star-disk and star-disk-halo
models, we derived inner ring-fit radii in the K band that are in the range of
0.8 - 1.6 AU. Additional temperature-gradient modeling resulted in an extended
disk with an inner radius of $0.67^{+0.51}_{-0.21}$ AU, a high inner
temperature of $2200^{+750}_{-350}$ K, and a disk inclination of
$53^{+15}_{-11}$$^\circ$.
  Conclusions: The derived geometric ring-fit radii are approximately 3 - 5
times smaller than that predicted by the size-luminosity relation. The small
geometric and temperature-gradient radii suggest optically thick gaseous
material that absorbs stellar radiation inside the dust disk.
