Chemical abundances and winds of massive stars in M31: a B-type supergiant and a WC star in OB10

We present high quality spectroscopic data for two massive stars in the OB10 association of M31, OB10–64 (B0 Ia) and OB10-WR1 (WC6). Medium resolution spectra of both stars were obtained using the ISIS spectrograph on the William Hershel Telescope. This is supplemented with HST-STIS UV spectroscopy and Keck I HIRES data for OB10–64. A non-LTE model atmosphere and abundance analysis for OB10–64 is presented indicating that this star has similar photospheric CNO, Mg and Si abundances as solar neighbourhood massive stars. A wind analysis of this early B-type supergiant reveals a mass-loss rate of Ṁ = 1.6×10M⊙yr , and v∞ = 1650kms . The corresponding wind momentum is in good agreement with the wind momentum – luminosity relationship found for Galactic early B supergiants. Observations of OB10-WR1 are analysed using a non-LTE, line-blanketed code, to reveal approximate stellar parameters of logL/L⊙ ∼5.7, T∗ ∼75kK, v∞ ∼ 3000kms , Ṁ/(M⊙yr ) ∼ 10 adopting a clumped wind with a filling factor of 10%. Quantitative comparisons are made with the Galactic WC6 star HD92809 (WR23) revealing that OB10-WR1 is 0.4 dex more luminous, though it has a much lower C/He ratio (∼0.1 versus 0.3 for HD92809). Our study represents the first detailed, chemical model atmosphere analysis for either a B-type supergiant or a WR star in Andromeda, and shows the potential of how such studies can provide new information on the chemical evolution of galaxies and the evolution of massive stars in the local Universe.