Shock Temperature at a Protoplanetary Disk Surface

Details Shock Temperature at a Protoplanetary Disk Surface Shock Temperature at a Protoplanetary Disk Surface

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..243i&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

Physics

Scientific paper

We did research on shock heating process at the disk surface due to gas accretion from a molecular cloud during formation of a protoplanetary disk. We compared various kinds of time scales in the post shock region both for gas and for dust grains because a physical process which has a shorter time scale dominates over in the post shock region. We have found that the temperature in the shocked gas decreases immediately because of dissociative cooling by hydrogen molecules, while dust grains cross the low density and high temperature region. Grains are heated in the higher density and cooler region by the gas drag heating.

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