  We present new coronagraphic images of Beta Pictoris obtained with the Space
Telescope Imaging Spectrograph (STIS) in September 1997. The high-resolution
images (0.1") clearly detect the circumstellar disk as close as 0.75" to the
star, corresponding to a projected radius of 15 AU. The images define the warp
in the disk with greater precision and at closer radii to Beta Pic than do
previous observations. They show that the warp can be modelled by the
projection of two components: the main disk, and a fainter component, which is
inclined to the main component by 4-5 degrees, and which extends only as far as
~4" from the star. We interpret the main component as arising primarily in the
outer disk and the tilted component as defining the inner region of the disk.
  The observed properties of the warped inner disk are inconsistent with a
driving force from stellar radiation. However, warping induced by the
gravitational potential of one or more planets is consistent with the data.
Using models of planet-warped disks constructed by Larwood and Papaloizou
(1997), we derive possible masses of the perturbing object.
