Spectroscopic and evolutionary analyses of the binary system AzV 14 outline paths toward the WR stage at low metallicity

D. Pauli, L. M. Oskinova, W. R. Hamann, D. M. Bowman, H. Todt, T. Shenar, A. A.C. Sander, C. Erba, V. M.A. Gómez-González, C. Kehrig, J. Klencki, R. Kuiper, A. Mehner, S. E. de Mink, M. S. Oey, V. Ramachandran, A. Schootemeijer, S. Reyero Serantes, A. Wofford

Research output: Contribution to journalArticlepeer-review

1 Scopus citations


Context. The origin of the observed population of Wolf-Rayet (WR) stars in low-metallicity galaxies, such as the Small Magellanic Cloud (SMC), is not yet understood. Standard, single-star evolutionary models predict that WR stars should stem from very massive O-type star progenitors, but these are very rare. On the other hand, binary evolutionary models predict that WR stars could originate from primary stars in close binaries. Aims. We conduct an analysis of the massive O star, AzV 14, to spectroscopically determine its fundamental and stellar wind parameters, which are then used to investigate evolutionary paths from the O-type to the WR stage with stellar evolutionary models. Methods. Multi-epoch UV and optical spectra of AzV 14 are analyzed using the non-local thermodynamic equilibrium (LTE) stellar atmosphere code PoWR. An optical TESS light curve was extracted and analyzed using the PHOEBE code. The obtained parameters are put into an evolutionary context, using the MESA code. Results. AzV 14 is a close binary system with a period of P = 3.7058 ± 0.0013 d. The binary consists of two similar main sequence stars with masses of M1,2 ≈ 32 M . Both stars have weak stellar winds with mass-loss rates of log Ṁ /(M yr−1) = −7.7 ± 0.2. Binary evolutionary models can explain the empirically derived stellar and orbital parameters, including the position of the AzV 14 components on the Hertzsprung-Russell diagram, revealing its current age of 3.3 Myr. The model predicts that the primary will evolve into a WR star with Teff ≈ 100 kK, while the secondary, which will accrete significant amounts of mass during the first mass transfer phase, will become a cooler WR star with Teff ≈ 50 kK. Furthermore, WR stars that descend from binary components that have accreted significant amount of mass are predicted to have increased oxygen abundances compared to other WR stars. This model prediction is supported by a spectroscopic analysis of a WR star in the SMC. Conclusions. Inspired by the binary evolutionary models, we hypothesize that the populations of WR stars in low-metallicity galaxies may have bimodal temperature distributions. Hotter WR stars might originate from primary stars, while cooler WR stars are the evolutionary descendants of the secondary stars if they accreted a significant amount of mass. These results may have wide-ranging implications for our understanding of massive star feedback and binary evolution channels at low metallicity.

Original languageEnglish
Article numberA40
JournalAstronomy and Astrophysics
StatePublished - 1 May 2023
Externally publishedYes


FundersFunder number
Gaia Data Processing and Analysis Consortium
Junta de Andalucía Excellence ProjectP18-FR-2664
State Agency for Research
National Aeronautics and Space AdministrationNAS 5-26555, NAG5-7584, 098.A-0049
Horizon 2020 Framework Programme
H2020 Marie Skłodowska-Curie Actions101024605
Space Telescope Science Institute
Diabetes Patient Advocacy Coalition
European Space Agency
Deutsche Forschungsgemeinschaft445674056, SA4064/1-1
Deutsches Zentrum für Luft- und Raumfahrt50OR2108, FKZ 50OR2005
Fonds Wetenschappelijk Onderzoek1286521N, KU 2849/9
Ministerio de Economía y CompetitividadAYA2016-79724-C4-4-P, PID2019-107408GB-C44
Lorentz Center
Instituto de Astrofísica de AndalucíaSEV-2017-0709
International Space Science Institute


    • binaries: close
    • binaries: eclipsing
    • binaries: spectroscopic
    • stars: early-type
    • stars: fundamental parameters
    • stars: individual: AzV 14


    Dive into the research topics of 'Spectroscopic and evolutionary analyses of the binary system AzV 14 outline paths toward the WR stage at low metallicity'. Together they form a unique fingerprint.

    Cite this