Radiative transfer in disk geometry - Emergent intensity from cool gray disks

Details Radiative transfer in disk geometry - Emergent intensity from cool gray disks Radiative transfer in disk geometry - Emergent intensity from cool gray disks

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icar...61...27s&link_type=abstract

(Conference on Protostars and Planets II, Tucson, AZ, Jan. 4-7, 1984) Icarus (ISSN 0019-1035), vol. 61, Jan. 1985, p. 27-35.

Statistics

Computation

4

Accretion Disks, Cosmic Dust, Disks (Shapes), Interstellar Matter, Radiative Transfer, Astronomical Models, Brightness Temperature, Graphite, Ray Tracing

Scientific paper

As part of a continuing project to develop self-consistent radiative transfer solutions in disk geometry, numerical models for disk shaped dust clouds are presented. Models are computed with the assumption of gray (Rosseland mean) opacity for cool, externally heated disks. For a given temperature distribution, based on a reasonable estimate for molecular clouds, or precollapse protoplanetary disks, the effect on the emergent intensity of disk geometry (i.e., degree of flattening), optical depth, and inclination to the observer's line of sight is examined. The goal of this research is to develop a computational tool for interpretation of observations of disk-shaped objects.

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