Resonance lines of C IV and N V form out to 316 solar radii in the wind of an O-type star, favoring a beta-law velocity exponent of 0.5 over the usual 0.8.
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2 Pith papers cite this work. Polarity classification is still indexing.
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New stable wind solutions fill the elusive gap between fast and δ-slow radiation-driven regimes, showing velocity kinks and distinct H I, He I, Si IV line profiles.
citing papers explorer
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First measurement of wind line formation regions in an early O-type star
Resonance lines of C IV and N V form out to 316 solar radii in the wind of an O-type star, favoring a beta-law velocity exponent of 0.5 over the usual 0.8.
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Radiation-driven stellar winds at the fast-slow transition: new hydrodynamic solutions
New stable wind solutions fill the elusive gap between fast and δ-slow radiation-driven regimes, showing velocity kinks and distinct H I, He I, Si IV line profiles.