Planetary embryos and planetesimals residing in thin debris discs

Details Planetary embryos and planetesimals residing in thin debris discs Planetary embryos and planetesimals residing in thin debris discs

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007mnras.380.1642q&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 380, Issue 4, pp. 1642-1648.

Astronomy and Astrophysics

Astronomy

11

Stars: Individual: Au Microscopii, Stars: Individual: Beta Pictoris, Stars: Individual: Fomalhaut, Planetary Systems: Formation, Planetary Systems: Protoplanetary Discs

Scientific paper

We consider constraints on the planetesimal population residing in the discs of AU Microscopii (AU Mic), β Pictoris (β Pic) and Fomalhaut taking into account their observed thicknesses and normal disc opacities. We estimate that bodies of radius 5, 180 and 70 km are responsible for initiating the collisional cascade accounting for the dust production for AU Mic, β Pic and Fomalhaut's discs, respectively, at break radii from the star where their surface brightness profiles change slope. Larger bodies, of radius 1000km and with surface density of the order of 0.01gcm-2, are required to explain the thickness of these discs assuming that they are heated by gravitational stirring. A comparison between the densities of the two sizes suggests the size distribution in the largest bodies is flatter than that observed in the Kuiper belt. AU Mic's disc requires the shallowest size distribution for bodies with radius greater than 10km suggesting that the disc contains planetary embryos experiencing a stage of runaway growth.

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