The mass discrepancy problem in O stars of solar metallicity. Does it still exist?

Abstract

Using own and literature data for a large sample of O stars in the Milky Way, we investigate the correspondence between their spectroscopic and evolutionary masses, and try to put constraints on various parameters that might influence the estimates of these two quantities.

arXiv comment4 pages, 2 figures, IAU Symposium 307, New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry, G. Meynet, C. Georgy, J.H. Groh \& Ph. Stee, eds

References in corpus (4)

• Masses and Luminosities of O and B - type stars and red super giants
• Measuring mass-loss rates and constraining shock physics using X-ray line profiles of O stars from the Chandra archive
• A Bake-Off Between CMFGEN and FASTWIND: Modeling the Physical Properties of SMC and LMC O-type Stars
• Photometric and Spectroscopic Studies of Massive Binaries in the Large Magellanic Cloud. I. Introduction and Orbits for Two Detached Systems: Evidence for a Mass Discrepancy?

Cited by in corpus (3)

• Accurate fundamental parameters and distance to a massive early-type eclipsing binary in the Danks 2 cluster
• Weighing stars from birth to death: mass determination methods across the HRD
• Properties of dwarf stars in Cygnus OB2