Astronomy and Astrophysics – Astronomy
Scientific paper
May 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000dda....31.0201t&link_type=abstract
American Astronomical Society, DDA Meeting #31, #02.01; Bulletin of the American Astronomical Society, Vol. 32, p.858
Astronomy and Astrophysics
Astronomy
Scientific paper
In formation stage of protoplanetary disk, shock waves are generated on the surface of the disk. As a result, dust particles existing in the infalling gas, as well as the gas itself, are heated by passing through the shock wave. In this study we investigated the shock heating of dust particles. A shock is composed of three regions: a preshock region, an intermediate thin region which is compressed adiabatically, and a post shock region. In the adiabatically compressed region, the gas temperature is very high ( > 6000 Kelvin), but the density is relatively low. In the post shock region, the temperature decreases (to a few hundred Kelvin) with an increase in the density through the radiative cooling of gas and dust particles. We investigated the evolution of the temperature of the dust particles in these regions by solving the gas-dust coupled momentum and the energy equations. The highest temperature of a dust particle is determined by the energy transfer between the gas and dust. We found that the heating rate of the dust particle in the adiabatically compressed region is smaller than it is in the post shock zone. In the post shock region, the temperature of a dust particle increases largely due to gas drag. We also find that the highest temperature of the dust particles, Td, increases with decreasing the particle size, rd, since the emissivity decreases for small dust particles. For example, Td is 1600K for rd=0.1 micron, while Td is 1000K for rd=1000 micron-sized dust in the case of that a shock wave generated in the asteroid region, where the gas velocity and density are 20 kms-1 and 1.2 x 10-14 gcm-3, respectively.
Horanyi Mihaly
Tanaka Kanenobu
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