AAS 201st Meeting, January, 2003
Session 56. Supernovae Potpourri
Poster, Tuesday, January 7, 2003, 9:20am-6:30pm, Exhibit Hall AB

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[56.04] Simulated Radio Images and Light Curves of Young Supernovae

V. V. Dwarkadas (ASCI Flash Center, Univ of Chicago), A. J. Mioduszewski ( National Radio Astronomy Observatory), L. Ball ( Australia Telescope National Facility, CSIRO)

We present calculations of the radio emission from supernovae based on high-resolution simulations of the hydrodynamics and radiation transfer, using simple energy density relations which link the properties of the radiating electrons and the magnetic field to the hydrodynamics. As a specific example we model the emission from SN1993J, which cannot be adequately fitted with the often-used analytic mini-shell model, and present a good fit to the radio evolution at a single frequency. Both free-free absorption and synchrotron self-absorption are needed to fit the light curve at early times and a circumstellar density profile of \rho ~r -1.7 provides the best fit to the later data. We discuss the use of high-resolution radio images of supernovae to distinguish between different absorption mechanisms and determine the origin of specific light curve features. Comparisons of VLBI images of SN1993J with synthetic model images suggest that internal free-free absorption completely obscures emission at 8.4 GHz passing through the center of the supernova for the first few tens of years after explosion. We predict that at 8.4 GHz the internal free-free absorption is currently declining, and that over the next ~40 years the surface brightness of the center of the source should increase relative to the bright ring of emission seen in VLBI images. Similar absorption in a nearby supernova would make the detection of a radio pulsar at 1 GHz impossible for ~150 years after explosion.

VVD is supported by the US. Department of Energy under grant number B341495 to the ASCI Flash Center at the University of Chicago.

The author(s) of this abstract have provided an email address for comments about the abstract: vikram@flash.uchicago.edu

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