Clumping in O-type Supergiants
We have analyzed the spectra of seven Galactic O4 supergiants, with the NLTE wind code CMFGEN. For all stars, we have found that clumped wind models match well lines from different species spanning a wavelength range from FUV to optical, and remain consistent with Hα data. We have achieved an excell...
| Main Authors: | , , , |
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| Format: | Others |
| Language: | English |
| Published: |
Universität Potsdam
2007
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| Subjects: | |
| Online Access: | http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17662 http://opus.kobv.de/ubp/volltexte/2008/1766/ |
| Summary: | We have analyzed the spectra of seven Galactic O4 supergiants, with the NLTE wind code CMFGEN. For all stars, we have found that clumped wind models match well lines from different species spanning a wavelength range from FUV to optical, and remain consistent with Hα data. We have achieved an excellent match of the P V λλ1118, 1128 resonance doublet and N IV λ1718, as well as He II λ4686 suggesting that our physical description of clumping is adequate. We find very small volume filling factors and that clumping starts deep in the wind, near the sonic point. The most crucial consequence of our analysis is that the mass loss rates of O stars need to be revised downward significantly, by a factor of 3 and more compared to those obtained from smooth-wind models. |
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