Orbital Motion of Resonant Clumps in Dusty Circumstellar Disks as a Signature of an Embedded Planet

Details Orbital Motion of Resonant Clumps in Dusty Circumstellar Disks as a Signature of an Embedded Planet Orbital Motion of Resonant Clumps in Dusty Circumstellar Disks as a Signature of an Embedded Planet

2000-05-17

arxiv.org/abs/astro-ph/0005347v1

Astronomy and Astrophysics

Astrophysics

5 pages, incl. 1 color figure, to appear in "Disks, Planetesimals, and Planets", conference held in Puerto de la Cruz, Tenerif

Scientific paper

We have applied a powerful numerical approach to compute, with a high resolution, the structure of dusty circumstellar disks with embedded planets. We emphasize some testable implications of our simulations which would verify the presence of a planet via thermal emission of one or more dusty clumps which are in mean motion resonances with the planet. In particular, our simulations indicate that Vega may have a massive planet of m~2 m_J (m_J being Jupiter's mass) at a distance of 50-60 AU, and Epsilon Eri may have a less massive planet of m~0.2 m_J at a similar distance of 55-65 AU. This conclusion is testable: Each resonant feature is stationary in the reference frame co-rotating with the planet, but it is not so for the observer at Earth. Therefore, if our interpretation of asymmetric clumps in circumstellar disks as dynamical resonant structures is correct, the above pattern revolves around the star with an angular velocity of (1.2-1.6) deg/yr (Vega) and (0.6-0.8) deg/yr (Epsilon Eri) -- a prediction that can be tested on a timescale of several years.

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