Use this URL to cite or link to this record in EThOS: http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.649907
Title: Infrared spectroscopy of Wolf-Rayet stars
Author: Eenens, P. R. J.
Awarding Body: University of Edinburgh
Current Institution: University of Edinburgh
Date of Award: 1992
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Abstract:
New high-resolution 1.0-34. μm spectra of carbon-rich Wolf-Rayet stars (WC) are presented. The line identifications are discussed and some 20 new identifications are given, due to neutral helium and ions of helium, carbon, oxygen and magnesium, notably the strong C IV 4p-4s doublet near 1.435 μm. It is shown that the infrared features are sufficient to define the subtypes, and that the optical classification lines refer to unrelated parameters: the ionization and the composition of the wind. Recombination lines are used to derive the C/He ratio in six WC and one WO stars. The validity of the assumptions is examined: the data are shown to be consistent with the lines being optically thin and formed by recombination; the increase in free-free optical depth with wavelength is used to estimate the effect of the wind stratification. The derived C/He ratios for WC stars are higher for earlier subtypes, they are much in excess over the solar value, and agree well with the results of other analyses. For the WO star, the C/He ratio is even higher, but lower than predicted by evolutionary models. Using new high-resolution spectra, the He I 2p-2s triplet and singlet profiles near 1.083 and 2.058 μm are analyzed, and shown to yield better estimates of the wind expansion velocity (v_∞) than conventional methods (based on the violet edge of ultraviolet resonance lines, or the width of optical emission lines). It is demonstrated that the velocities from the absorption trough of ultraviolet resonance P Cygni lines are contaminated by the companion O-star wind in WR+ O binaries. The infrared He I profiles are fitted to derive v_∞ in a sample of 41 galactic WR stars of all subtypes. The derived v_∞ tend to be higher in earlier subtypes. In general they are lower than those from the other methods, implying that the previous estimates of the mass-loss rates are also too high. The presence of emission subpeaks on the infrared He I lines is noted for the first time. These are widespread among WR stars, regardless of the subtype or the presence of an O-star companion. The subpeaks are believed not to vary with time and are suggested to be the signature of asymmetries in the wind.
Supervisor: Not available Sponsor: Not available
Qualification Name: Thesis (Ph.D.) Qualification Level: Doctoral
EThOS ID: uk.bl.ethos.649907  DOI: Not available
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