Statistics – Computation
Scientific paper
Feb 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...289..660c&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 289, Feb. 15, 1985, p. 660-668.
Statistics
Computation
17
Line Spectra, Magnetic Stars, Peculiar Stars, Spectral Energy Distribution, Stellar Atmospheres, Stellar Models, A Stars, Abundance, Atmospheric Pressure, Magnetic Field Configurations, Main Sequence Stars, Radiant Flux Density, Stellar Temperature, Zeeman Effect
Scientific paper
Magnetic, line-blanketed model atmospheres for upper-main-sequence stars with normal elemental abundances and a slightly distorted dipolar magnetic field have been constructed. These were computed with a modified version of the Kurucz ATLAS6 model atmosphere code and newly computed opacity distribution functions (ODFs), which take into account the Zeeman splitting of the contributing atomic lines. The inclusion of magnetic forces changes the structure of an atmosphere by altering the net gravity and thus the pressure distribution in the upper layers of the atmosphere. These magnetic forces cause the structure of the stellar model to vary with latitude and to differ from the nonmagnetic case. The enhanced blanketing represented by the 'magnetic' ODFS in combination with the structure changes and Zeeman broadening of individual lines causes the emergent spectrum to vary with viewing inclination and to differ from the nonmagnetic case. The structure and spectrum computations are described and results compared with those for nonmagnetic models. The results are discussed in light of existing observations of Ap stars, which are thought to have magnetic field configurations similar to the ones included in these models.
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