Prospects for Detection of Catastrophic Collisions in Debris Disks

Details Prospects for Detection of Catastrophic Collisions in Debris Disks Prospects for Detection of Catastrophic Collisions in Debris Disks

2005-03-24

arxiv.org/abs/astro-ph/0503551v1

Astron.J.130:269-279,2005

Astronomy and Astrophysics

Astrophysics

Astronomical Journal, in press; 23 pages of text, 11 figures, and 1 table

Scientific paper

10.1086/430461

We investigate the prospects for detecting dust from two body collisions during the late stages of planet formation at 1-150 AU. We develop an analytic model to describe the formation of a dusty cloud of debris and use numerical coagulation and n-body calculations to predict observable signals from these events. In a minimum mass solar nebula, collisions of 100-1000 km objects at distances of 3-5 AU or less from the parent star are observable at mid-infrared wavelengths as bright clumps or rings of dust. At 24 microns, the clumps are roughly 0.1-1 mag brighter than emission from dust in the background debris disk. In edge-on systems, dusty clumps produce eclipses with depths of 1.0 mag or less that last for roughly 100 orbital periods. Large-scale surveys for transits from exosolar planets, such as Kepler, can plausibly detect these eclipses and provide important constraints on the terrestrial environment for ages of less than or roughly 100-300 Myr.

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