Brightness distribution for resonant line photons in spherical envelopes

Details Brightness distribution for resonant line photons in spherical envelopes Brightness distribution for resonant line photons in spherical envelopes

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...158..310n&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 158, no. 1-2, April 1986, p. 310-324. Research supported by the Alfred P. Sloa

Statistics

Computation

15

Brightness Distribution, Computational Astrophysics, Line Spectra, Optical Resonance, Photons, Stellar Envelopes, Density Distribution, Monte Carlo Method, Radiative Transfer

Scientific paper

The scattering of resonant line photons in spherically symmetric, expanding envelopes with turbulence is studied numerically using a Monte-Carlo scattering code. The envelopes have different radial density distributions for scatterers, various ratios of systematic to random velocity, and different line center optical depths. These calculations produce both emerging line profiles and spatial brightness distributions for scattered photons as they appear to a distant observer. The line shapes and brightness distributions are weak functions of line center optical depth and the form of the density distribution, being virtually indistinguishable for a wide range of parameters. Differing ratios of systematic to random velocity have a stronger effect on the emerging photons. The authors argue that although it may be difficult to determine densities and temperatures in circumstellar envelopes from spectral line data, it will be easier to detect velocity gradients, especially when brightness data become available.

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