Electron scattering in the atmospheres of hot DA white dwarfs

Astronomy and Astrophysics – Astrophysics

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Electron Scattering, Hot Stars, Stellar Atmospheres, Stellar Radiation, White Dwarf Stars, Atmospheric Models, Extreme Ultraviolet Radiation, Optical Thickness

Scientific paper

High-frequency emission from the photosphere of hot, hydrogen-rich white dwarfs is reexamined, taking into account results of Bohm and Kapranidis (1980), which state that electron scattering has a strong influence on the energy distribution at EUV wavelengths. Calculations made with and without electron scattering indicate that scattering does not have significant influence for frequencies below 2 x 10 to the 16th Hz. Emission is enhanced at high frequencies without scattering due to the lower opacity in the atmosphere which implies that continuum formation occurs much deeper in the atmosphere in hotter layers. Results indicate that electron scattering dominates the source function over a long range of depths, and support Shipman's (1979) explanation that the EUV flux arises from thermal emission from hot, deep-lying photospheric layers.

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