Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...305..541c&link_type=abstract
Astronomy and Astrophysics, v.305, p.541
Astronomy and Astrophysics
Astrophysics
57
Stars: Abundances, Stars: Wr 134, Wr 136, Stars: Wolf-Rayet, Stars: Mass-Loss, Infrared: Stars
Scientific paper
We investigate whether the stellar parameters and chemistries of Wolf-Rayet stars can be adequately determined from IR observations by focusing on two WN 6 stars which have been the subject of numerous optical studies. Our analysis is based on new UKIRT-CGS4 observations of the strong, broad-lined stars WR 134 (HD191765) and WR 136 (HD192163) in Cygnus. We find excellent agreement in our derived stellar parameters for both stars (T_*_~55kK, T_2/3_~29kK, logL/Lsun_~5.3, log˙(M)/Msun_/yr~-3.9, vinfinity_~1900km/s) with previous optical tailored analyses (e.g. Hamann et al. 1994). The numerous unblended H and He emission lines in the IR allow us to determine very accurate H/He ratios for these two stars. We confirm that WR 136 contains substantial hydrogen (~10% by mass) while less than 1% hydrogen is found for WR 134. We provide a spectral comparison of WN 3-9 stars in the I, H and K-bands and give theoretical intrinsic WN infrared colours of use for future IR studies. We note that the WN 9 star WR 105 (NS4) has a similar spectral morphology to the Galactic Centre helium emission stars (Allen et al. 1990; Krabbe et al. 1991). We also present synthetic 2.5-10μm spectra of WR 136 for comparison with planned ISO spectroscopic observations.
Crowther Paul A.
Smith Lleweilun J.
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