Statistics – Computation
Scientific paper
Nov 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981sao..reptq....d&link_type=abstract
Semiannual Report, 1 Apr. - 30 Sep. 1981 Smithsonian Astrophysical Observatory, Cambridge, MA.
Statistics
Computation
Chromosphere, Cool Stars, Cooling, Radiative Transfer, Stellar Temperature, Stellar Winds, Atmospheric Temperature, Computer Programs, Stellar Atmospheres, Stellar Gravitation, Supergiant Stars, Wind Velocity
Scientific paper
Calculated radiative losses from H, H-, Ca II, and Mg II show that cooling for the chromosphere of the supergiant epsilon Gem do not differ greatly from the solar law, although there are differences at approximately 6000K due to ionization effects. With a rough standard law for computation of stellar winds using the Hartmann-MacGregor theory and standard stellar evolutionary calculations, the wind velocities and temperatures in the HR diagram were systematically explored. Results show that cool winds with tempratures 1,000,00K are not possible for log g or = 2. Predicted wind velocities are approximately 1.5 to 2 x larger than observed, particularly for the most luminous cool stars. The ionization balance for the wind of alpha ORI and the hydrogen profile lines for T Tauri stars were computed using the PANDORA computer program.
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