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- W1886608386 abstract "A compact star in a detached binary system can accrete the matter from the stellar wind of the companion. In this case a more or less radial accretion flow is formed. By analogy to stellar winds from early type stars it is usually believed that the accretion of this sort should produce inverse P-Cygni profiles in resonance lines. However, there are physical differences between the wind and the radial accretion which can alter the outgoing profile significantly.KeywordsLine ProfileOptical ThicknessResonance LineStellar WindCompact StarThese keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves." @default.
- W1886608386 created "2016-06-24" @default.
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- W1886608386 date "1988-01-01" @default.
- W1886608386 modified "2023-09-27" @default.
- W1886608386 title "Resonance Line Profiles from Radial Accretion Flows" @default.
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- W1886608386 doi "https://doi.org/10.1007/978-94-009-2969-2_22" @default.
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