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A probabilistic approach to radiative energy loss calculations for optically thick atmospheres: Hydrogen lines and continua

Journal Article · · Astrophys. J.; (United States)
DOI:https://doi.org/10.1086/158193· OSTI ID:6735465
;
We simultaneously solve an approximate probabilistic radiative transfer equation and the statistical equilibrium equations for a model hydrogen atom consisting of three bound levels and ionization continuum. We explicitly solve the transfer equation for L..cap alpha.., L..beta.., H..cap alpha.., and the Lyman continuum, assuming complete redistribution. We have tested the accuracy of this approach by comparing source functions and radiative loss rates to values obtained with a method that solves the exact transfer equation. Two recent model solar-flare chromospheres are used for this test. We show that for the test atmospheres the probabilistic method gives values of the radiative loss rate that are characteristically good to a factor of 2. The advantage of this probabilistic approach is that it retains a description of the dominant physical processes of radiative transfer in the complete redistribution case, yet it achieves a major reduction in computational requirements.
Research Organization:
Center for Astrophysics and Space Science, University of California San Diego
OSTI ID:
6735465
Journal Information:
Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 239:3; ISSN ASJOA
Country of Publication:
United States
Language:
English

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Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
ATOMIC MODELS
CHROMOSPHERE
ELEMENTARY PARTICLES
ELEMENTS
ENERGY LEVELS
ENERGY LOSSES
HYDROGEN
IONIZATION
LOSSES
LYMAN LINES
MASSLESS PARTICLES
MATHEMATICAL MODELS
NONMETALS
PHOTONS
PROBABILITY
RADIATION EFFECTS
RADIATION TRANSPORT
SOLAR ACTIVITY
SOLAR ATMOSPHERE
SOLAR FLARES
STELLAR ATMOSPHERES
STELLAR RADIATION