Protoplanetary Disc Properties in Isolated and Binary Systems

Details Protoplanetary Disc Properties in Isolated and Binary Systems Protoplanetary Disc Properties in Isolated and Binary Systems

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008epsc.conf..798h&link_type=abstract

European Planetary Science Congress 2008, Proceedings of the conference held 21-25 September, 2008 in Münster, Germany. Online a

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Scientific paper

ABSTRACT With high resolution, multi-scale 3D SPH simulations using GASOLINE we follow the formation of a protostellar disc from the collapse of a turbulent molecular cloud core, and its subsequent evolution. Shortly after the formation of the first protoplanetary disc, the gas filament from which it accretes fragments, forming a companion. Another simulation with a slightly different turbulent velocity field produces an isolated disk instead, with a nearly identical environmental properties. We follow both the isolated and binary systems as they continue to accrete, and quantify the evolution of their disc properties, dynamics and thermodynamics within their natal environment. We find that the evolution of the disk mass, size, angular momentum and its eventual fragmentation into brown-dwarf sized companions are all affected by their being in a binary or in isolation. We then connect the different disk properties to their potential for planet formation.

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