[Previous] | [Session 128] | [Next]
S. D. Doty (Denison University)
A key to constraining the physical and chemical conditions in regions of star formation and stellar evolution is the comparison of high quality observations to detailed models of these regions. Recent (e.g., ISO, SWAS), and upcoming (e.g., FIRST, SOFIA) observatories will make high quality data available, with complimentary wavelength coverages, spatial resolutions, and spectral resolutions.
Detailed models are required to help interpret these data. Previous models have included arbitrary temperature, density, velocity, and chemical abundance gradients (e.g. Doty & Neufeld, 1997). However, observations (e.g. Dickman et al. 1990, Falgarone et al. 1991) also suggest irregular morphology due clumping and fragmentation in real sources.
Toward this end, we have begun modeling the radiation emitted by truly three-dimensional sources. In this first phase, we consider the thermal balance of the gas. We find that this is a computationally large, but soluble problem. We discuss our methodology and present results from our models, including test cases used for validation.
This work has been supported by an award from the Research Corporation.