A Revised Temperature Scale for Massive Stars

Details A Revised Temperature Scale for Massive Stars A Revised Temperature Scale for Massive Stars

Jul 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007uasb.conf..101b&link_type=abstract

UV Astronomy: Stars from Birth to Death. Proceedings of the Joint Discussion n.4 during the IAU general Assembly of 2006. Ana I.

Astronomy and Astrophysics

Astronomy

2

Uv Spectroscopy, Optical Spectroscopy, Hot Massive Stars, Stellar Parameters, Mass Loss

Scientific paper

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

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