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Near-Infrared Photometry of Southern Galactic Wolf-Rayet Stars

Published online by Cambridge University Press:  14 August 2015

C. Sterken  and
C. de Loore
C. Sterken
Affiliation:
Astrophysical Institute, Vrije Universiteit Brussel, Belgium
C. de Loore
Affiliation:
Astrophysical Institute, Vrije Universiteit Brussel, Belgium

Extract

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Allen et al. (1972) observed 40 WR stars in the |1.6µ| and |2.2µ| bands, and found evidence of interstellar dust emission in the WC9 stars Ve 2–45, AS320 and HD 313643. Hackwell et al. (1974) reported 2.3 to 23 µ photometry of 19 WR stars and concluded that the excess infrared radiation from the Wolf-Rayet stars (except for the WC9 stars) could be explained by free-free emission from a hot circumstellar shell. Gehrz and Hackwell (1974) found from 2.3 to 23 µ photometry that three out of four WC stars appear to be embedded in thick circumstellar dust (graphite) shells, and concluded that WC9 stars may form a distinct Wolf-Rayet class. Cohen et al. (1975) derived energy distributions of 23 Wolf-Rayet stars from 3µ-11µ scanner spectrophotometry and infrared photometry, and concluded that WN stars show only free-free emission whereas only WC stars show dust. The excesses in WC9 stars are interpreted as thermal emission by graphite grains.

Type
SESSION 1 — THE WOLF-RAYET PHENOMENON
Information
Symposium - International Astronomical Union , Volume 99: Wolf-Rayet Stars: Observations, Physics, Evolution , 1982 , pp. 67 - 72
Copyright
Copyright © Reidel 1982 

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