Signatures of exosolar planets in dust debris disks

We apply our recently elaborated, powerful numerical approach to the high-r esolution modeling of the structure and emission of circumstellar dust disk s, incorporating all relevant physical processes. Specifically, we examine the resonant structure of a dusty disk induced by the presence of one plane t. It is shown that the planet, via resonances and gravitational scattering , produces (1) an asymmetric resonant dust belt with one or more clumps, in termittent 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 i n the circumstellar dust disk and, moreover, can be used to determine its m ajor orbital parameters and even the mass of the planet. The results of our study reveal a remarkable similarity with various types of highly asymmetr ic circumstellar disks observed with the James Clerk Maxwell Telescope arou nd epsilon Eridani and Vega. The proposed interpretation of the clumps in t hose disks as being resonant patterns is testable-it predicts the asymmetri c design around the star to revolve, viz., by 1.degrees 2-1.degrees 6 yr(-1 ) about Vega and 0.degrees 6-0.degrees 8 yr(-1) about epsilon Eri.