Transfer of resonant line photons in spherically accelerating envelopes

Details Transfer of resonant line photons in spherically accelerating envelopes Transfer of resonant line photons in spherically accelerating envelopes

Jul 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...181...57b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 181, no. 1, July 1987, p. 57-70. Research supported by the Alfred P. Sloan Fou

Astronomy and Astrophysics

Astrophysics

6

Light Scattering, Photons, Resonance Lines, Stellar Envelopes, Stellar Rotation, Brightness, Monte Carlo Method, Stellar Atmospheres, Stellar Models, Turbulent Flow

Scientific paper

Numerical calculations of the scattering of resonance photons in spherically symmetric, outward accelerating envelopes with turbulence are used to discuss common features of the line shapes and brightness distributions. The velocity and density distributions of scatterers encompass most of the forms proposed for different mass-loss processes from stellar atmospheres. For moderate-to-low optical depths, the line shapes depend strongly on the velocity and density profiles. The brightness distributions integrated over the line profiles tend to be confined to spheres of less than two stellar radii and are rather insensitive to the envelope parameters. Photons scattered in the red and blue wings of the frequency profile have broad brightness distributions whose widths reflect the positions of acceleration regions within the envelopes. The results suggest that it will be straightforward to detect velocity gradients and to locate acceleration regions in an envelope by using line profiles and brightness data with both high spatial and spectral resolution.

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