Cooling, Sputtering, and Infrared Emission from Dust Grains in Fast Shocks

Details Cooling, Sputtering, and Infrared Emission from Dust Grains in Fast Shocks Cooling, Sputtering, and Infrared Emission from Dust Grains in Fast Shocks

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...183.1404f&link_type=abstract

American Astronomical Society, 183rd AAS Meeting, #14.04; Bulletin of the American Astronomical Society, Vol. 25, p.1310

Astronomy and Astrophysics

Astrophysics

Scientific paper

We model the dynamics, the destruction by sputtering and the collisional heating of dust grains in fast (>= 400 \ km \ s(-1) ) astrophysical shocks. The effect of grain destruction is to alter the grain size distribution, creating a deficiency of small grains compared to their preshock abundances. The altered grain size distribution depends on shock velocity and the density of the ISM. We calculate the infrared emission from the dust particles using a stochastic dust heating model (Dwek, 1986). In this model, particles with sizes below ~ 100 A undergo temperature fluctuations and radiate an excess of near infrared emission (lambda <= 20 \ microns ) over that expected for grains in thermal equilibrium. The near infrared excess is a measure of the abundance of small grains in the shock, and the infrared spectrum is, therefore, a powerful diagnostic for the amount of grain destruction in shocks. These studies compliment those that examine the effects of the release of the sputtered refractory elements on the ultraviolet and X-ray emission from shocks (Vancura, et al. 1993). Dwek, E. 1986, ApJ, 302, 363. Vancura, O., Raymond, J.C., Dwek, E., Blair, W.P., Long, K.S., and Foster, S., 1993, in preparation. This work is funded by NASA RTOP #188-44-53-05.

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