No Title In Schaerer et al. The atmosphere models include line blanketing for all elements from hydrogen to zinc. These results may, e.g., be used for population synthesis models intended to study the massive star content in young starforming regions. Particular emphasis is given to comparisons of the UV spectral evolution with observations, including continuum indices and several metal line signatures of P-Cygni lines and broad absorption features.
Good agreement is found for most UV features.
A feature in late O and early B giants and supergiants. This feature is found to depend sensitively on temperature and may be used to derive effective temperatures for these stars.