A Revised Temperature scale for Massive Stars

Details A Revised Temperature scale for Massive Stars A Revised Temperature scale for Massive Stars

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...4e..36b&link_type=abstract

The Ultraviolet Universe: Stars from Birth to Death, 26th meeting of the IAU, Joint Discussion 4, 16-17 August 2006, Prague, Cze

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Scientific paper

A consistent analysis, using non-LTE codes with sphericity and mass loss, of different ionization species in O star spectra observed from the far-UV to UV allowed us to constrain the long-time uncertain ionization equilibrium in the stellar winds, to quantify the role of soft X-rays from shocks and to reconcile otherwise discrepant UV line diagnostics. The modelling initially performed with the WM-basic code led to a revised (downwards) Teff scale for Galactic O-type stars, a result with important implications for the energy-balance calculations in HII regions and for massive star evolution. A further analysis using the CMFGEN code, including clumping effects, allowed us to resolve the remaining UV line discrepancies, in particular the PV line in the far-UV, and to finally reconcile mass loss and photospheric parameters derived from optical and UV lines.

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