IMPROVED BOLOMETRIC CORRECTIONS FOR WR STARS

Evolutionary models allow an assignment of both a mass and a luminosit y to a Wolf-Rayet (WR) star in a cluster, and hence allow a determinat ion of the Bolometric Correction (B.C.). The B.C.'s derived for WN sta rs range from -4.0 to -6.0 with the expected trend of larger values (i n absolute values) for stars with higher excitation spectra. For WC st ars, there is little evidence for a similar trend; most observations p resented here are consistent with B.C. = -4.5, as found by Smith and M aeder (1989). The convergence of B.C. values derived from evolutionary and atmospheric models is extremely satisfactory, giving increased co nfidence in both methods.