Other
Scientific paper
Feb 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993kfnt....9q...3a&link_type=abstract
Kinematika i Fizika Nebesnykh Tel (ISSN 0233-7665), vol. 9, no. 1, p. 3-15.
Other
3
Hydrodynamic Equations, Photosphere, Solar Atmosphere, Three Dimensional Models, Method Of Moments, Numerical Integration, Radiative Transfer, Spectral Energy Distribution
Scientific paper
A numerical algorithm is presented for calculation of the three-dimensional hydrodynamic stellar photospheric models based on the second-order scheme for integration of a system of hydrodynamic equations. The momentum method is used to solve the radiation energy transfer equation in the three-dimensional medium, the energy transport in the spectral lines being taken into account. A sequence of hydrodynamic models of the solar photosphere is computed using this algorithm. The results of the numerical simulation are compared with those obtained by other authors. Computed models reproduce the observed features of the fine structure of the solar Fraunhofer lines. The intensity fluctuations calculated are about 17 percent for 500-nm wavelength and about 12 percent for 600-nm wavelength in the solar disk center.
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