Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...102...73h&link_type=abstract
Astronomy and Astrophysics, vol. 102, no. 1, Sept. 1981, p. 73-80. Research supported by the Deutsche Forschungsgemeinschaft.
Astronomy and Astrophysics
Astrophysics
32
B Stars, Colorimetry, Stellar Evolution, Stellar Temperature, Atmospheric Models, Interstellar Extinction, Line Spectra, Stellar Atmospheres
Scientific paper
Johnson and Stromgren colors, including reddening lines, have been computed for extreme helium stars using a grid of unblanketed model atmospheres. Effective temperatures are determined from the observed colors for all the known extreme helium stars. Stromgren colors were better suited than Johnson colors in order to determine the effective temperatures of the helium stars, and were also less dependent on the calibration system. From the statistics of the effective temperatures, it is concluded that the extreme helium stars evolve to higher effective temperatures and finally cool down to become white dwarfs. Using the evolutionary tracks of Schoenberner (1977), it is found that the temperature increase corresponds to a time interval of approximately 40 years for a mass of 0.7 solar mass and approximately 300 years for a mass of 1.0 solar mass.
Heber Uli
Schoenberner Detlef
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