Debris Disc Stirring by Giant Planets

Details Debris Disc Stirring by Giant Planets Debris Disc Stirring by Giant Planets

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dda....41.1002m&link_type=abstract

American Astronomical Society, DDA meeting #41, #10.02; Bulletin of the American Astronomical Society, Vol. 41, p.938

Astronomy and Astrophysics

Astronomy

Scientific paper

Detectable debris discs are thought to require dynamical excitation (`stirring'), so that planetesimal collisions release large quantities of dust. We investigate the effects of the secular perturbations of a planet, which may lie at a significant distance from the planetesimal disc, to see if these perturbations can stir the disc, and if so over what time-scale. The secular perturbations cause orbits at different semi-major axes to precess at different rates, and after some time initially non-intersecting orbits begin to cross. We derive an expression for this time-scale in terms of the mass, eccentricity, and semi-major axis of the planet, and the semi-major axis of the disc. This time-scale can be faster than that for the growth of planetesimals to Pluto's size within the outer disc. We also calculate the magnitude of the relative velocities induced amongst planetesimals and infer that a planet's perturbations can typically cause destructive collisions out to 100's of AU. Recently formed planets can thus have a significant impact on planet formation in the outer disc which may be curtailed by the formation of giant planets much closer in. The presence of an observed debris disc does not require the presence of Pluto-sized objects within it, since it can also have been stirred by a planet not in the disc. As an example we consider the star epsilon Eridani, and we find that the known RV planet can excite the planetesimal belt at 60 AU sufficiently to cause destructive collisions of bodies up to 50 km in size, on a time-scale of 40 Myr.
The support of an STFC studentship is gratefully acknowledged.

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