Numerical calculations of radiation transport in a dusty medium in disk geometry

Details Numerical calculations of radiation transport in a dusty medium in disk geometry Numerical calculations of radiation transport in a dusty medium in disk geometry

Sep 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986phdt.........5s&link_type=abstract

Ph.D. Thesis Rensselaer Polytechnic Inst., Troy, NY.

Astronomy and Astrophysics

Astrophysics

1

Angular Momentum, Astronomical Models, Newton-Raphson Method, Radiation Transport, Star Formation, Geometry, Optical Properties, Radiation Distribution

Scientific paper

Both theoretical and observational evidence suggest that nonspherical geometries should be invoked to describe many astrophysical sources. Geometries dominated by considerations of angular momentum are favored by current models of the star formation process. Radiation transport in the two-dimensional coordinates appropriate to disk geometry was studied. The approach used is to recast the transport equation in second-order form by using a series of angular momentums of the radiation field, and by the introduction of a set of auxillary functions dependent on the geometry and on the anisotropy of the radiation field. The resulting system of equations is solved by Newton-Raphson iteration to yield a self-consistent temperature and mean intensity for each point in the disk, under the assumptions of radiative equilibrium and complete isotropy of the radiation field. Detailed angular variations of the local radiation field, and of the emergent intensity are recovered by tracing a set of rays through the disk. This technique was applied to model a set of disk-shaped, quiescent dust clouds, using realistic optical properties for the assumed grain mixture, and using an ambient external radiation field consistent with that observed in the solar neighborhood.

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