Turbulent Motions with Finite Correlation Length in the Winds of K and M Supergiants

Details Turbulent Motions with Finite Correlation Length in the Winds of K and M Supergiants Turbulent Motions with Finite Correlation Length in the Winds of K and M Supergiants

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003csss...12.1058b&link_type=abstract

The Future of Cool-Star Astrophysics: 12th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (2001 July 30 - August

Astronomy and Astrophysics

Astrophysics

Line Formation

Scientific paper

High resolution spectra of lines formed in the wind of evolved late-type stars suggest that the usual microturbulent assumption is not adequate to describe the nonthermal motions. We present a NLTE radiative transfer scheme that incorporates turbulent velocity fields with finite correlation length. In this approach we consider the turbulent velocity and consequently the intensity to be stochastic variables. This leads to a generalized equation of transfer having the form of a Fokker-Planck equation. In a first application we demonstate the general effects of velocity fluctuations on the line formation in expanding atmospheres.

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