A line driven Rayleigh-Taylor-type instability in hot stars

Details A line driven Rayleigh-Taylor-type instability in hot stars A line driven Rayleigh-Taylor-type instability in hot stars

Apr 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978a%26a....65..223n&link_type=abstract

Astronomy and Astrophysics, vol. 65, no. 2, Apr. 1978, p. 223-227.

Astronomy and Astrophysics

Astrophysics

26

Atmospheric Heating, Hot Stars, Line Spectra, Taylor Instability, Chromosphere, Coronas, Optical Resonance, Stellar Spectra, Stellar Winds, Wind Velocity

Scientific paper

The existence of a Rayleigh-Taylor-type instability in the atmospheres of hot stars, driven by the radiative force associated with impurity ion resonance lines, is demonstrated. In a hot star with an effective temperature of 50,000 K, the instability will grow exponentially with a time scale of approximately 50 s in the layers where the stellar wind velocity is 5% of the thermal velocity of the ion. As a result, radially symmetric stellar winds driven by resonance line radiative forces will break up in small horizontal scale lengths. The energy fed into the instability provides a possible source of mechanical heating in the atmosphere for a chromosphere or corona.

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