Statistics – Computation
Scientific paper
Apr 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...159...90l&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 159, no. 1-2, April 1986, p. 90-100.
Statistics
Computation
37
Balmer Series, Radiation Pressure, Stellar Mass Ejection, Stellar Winds, Supergiant Stars, Computational Astrophysics, Hertzsprung-Russell Diagram, Iue, Stellar Luminosity, Ultraviolet Spectra
Scientific paper
The acceleration of the wind of P Cygni between 1.1 R* and 4 R* is derived from the velocity law. The acceleration is due to an outward directed force, which barely exceeds the gravity and varies approximately as r-1.8. The acceleration can be explained by radiation pressure due to a very large number (≡103) of weak lines in the Balmer continuum. These lines have been observed in the IUE spectra. The authors propose that the mass loss of P Cygni type stars and the luminosity upper limit in the HR-diagram is due to radiation pressure by weak metal lines in the Balmer continuum. This will produce an instability limit at Teff ⪉ 30,000K when geff ⪉ 102cm/s2.
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