  We apply our recently elaborated, powerful numerical approach to the
high-resolution modeling of the structure and emission of circumstellar dust
disks, incorporating all relevant physical processes. Specifically, we examine
the resonant structure of a dusty disk induced by the presence of one planet.
It is shown that the planet, via resonances and gravitational scattering,
produces (1) an asymmetric resonant dust belt with one or more clumps
intermittent with one or a few off-center cavities; and (2) a central cavity
void of dust. These features can serve as indicators of a planet embedded in
the circumstellar dust disk and, moreover, can be used to determine its major
orbital parameters and even the mass of the planet. The results of our study
reveal a remarkable similarity with various types of highly asymmetric
circumstellar disks observed with the James Clerk Maxwell Telescope around
Epsilon Eridani and Vega. The proposed interpretation of the clumps in those
disks as being resonant patterns is testable -- it predicts the asymmetric
design around the star to revolve, viz., by 1.2--1.6 deg/yr about Vega and
0.6--0.8 deg/yr about Epsilon Eri.
