Self-consistent models of the dusty content of protoplanetary disk: modelisation and observations

Details Self-consistent models of the dusty content of protoplanetary disk: modelisation and observations Self-consistent models of the dusty content of protoplanetary disk: modelisation and observations

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010lyot.confe..28c&link_type=abstract

Proceedings of the conference In the Spirit of Lyot 2010: Direct Detection of Exoplanets and Circumstellar Disks. October 25 -

Physics

Scientific paper

Today we reach apoint where multiwavelenght observations (Spitzer, Herschel, ALMA) provide (or will provide) critical constraints on the dust content of gaseous protoplanetary disls. However, the dusty content of these disks is rapidly evolving under the action of dynamical effects (sedimentation, migration) and physical effects (coagulation, fragmentation), making observations very difficult to interpret unambiguously. In particular, the coupling of dynamical and collisiona effect is expected to produce peculiar distribution of dust, highly dependdant on the distance, on the temperature and density profile of the disk,that has been poorly investigated, due to the difficulty of coupling such various processes. In the present work we show results of a new code (Charnoz et al., 2010) able to combine self-consistently collisional processes and dynamical processes, in a 3D way. We are now able to derive the size distribution of dust present in the disks' photospheres, and compare it to the size distribution of solid content the midplane. We will show how small dust (<1 mic.) may be used as a tracer of larger bodies accreting in the midplance, and also how out-of equilibrium coagulation (i.e. on timescales smaller that the gas friction time), may lead to the formation of meter-sized bodies.

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