Keplerian Masses for the Most Massive Stars: The Very Luminous, Hydrogen-Rich Wolf-Rayet Stars

Details Keplerian Masses for the Most Massive Stars: The Very Luminous, Hydrogen-Rich Wolf-Rayet Stars Keplerian Masses for the Most Massive Stars: The Very Luminous, Hydrogen-Rich Wolf-Rayet Stars

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...5e...1m&link_type=abstract

Calibrating the Top of the Stellar M-L Relation, 26th meeting of the IAU, Joint Discussion 5, 16 August 2006, Prague, Czech Repu

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Locating the most massive stars and measuring their masses is key to understanding the formation and nature of massive stars in general. This is best done by using the least model-dependent technique, i.e. Kepler's laws (combined with techniques to extract the orbital inclination) for binary systems that contain very luminous stars on or near the main sequence, where interaction effects are not (yet) important. In the local Universe, it appears that the potentially most massive, main-sequence stars are the most luminous hydrogen-rich WR stars of type WN5-7ha, which are even more luminous than, and probably at least as hot as, the recently recognized hottest main-sequence stars of type O2. WN5-7ha stars exhibit strong, broad WR-like emission lines because of their high luminosity, not because of their compactness and high ratio of L/M as classical He-burning, WR stars. It is probably no coincidence that the currently most massive stars measured this way are in WR20a, an eclipsing binary system containing two identical WN6ha stars of 83 and 82 solar masses. Other WN5-7ha stars, some even more luminous than WR20a, are being measured currently and I will report on the overall results, with implications for stellar evolution.

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