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Eclipsing binaries

laboratories. for testing. rotational mixing. Selma de Mink. Matteo Cantiello ... Selma de Mink. Liege July 8th, 2008. S. E. de Mink @ uu.nl. Very Massive ...

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Eclipsing binaries

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    1. Eclipsing binaries as laboratories for testing rotational mixing

    Selma de Mink Matteo Cantiello* Norbert Langer* Ines Brott* Onno Pols Evert Glebbeek* Sung-Chul Yoon Mark Verkoulen S.E.deMink@uu.nl Astronomical Institute Utrecht The Netherlands

    2. Motivation

    Independent tests needed VLT-flames: massive stars survey Eclipsing binaries Evans+, Hunter+, Brott+

    3. Single stellar models

    with rotational mixing

    Pspin= 1.4 days Pspin= 2.7 days Pspin= 0.9 days ) Age (yr)? Surface N abun.

    4. Single stellar models

    Based on models by Yoon+06 Porbit= 1.4 days Porbit= 2.7 days Porbit= 0.9 days Tight binary ? Tidal locking: Pspin = Porbit

    5. Binary models

    with rotational mixing

    6. Binaries

    ) Age (Myr)? Surface N abun. De Mink & Cantiello,+ (in prep.)? 0 2 4 6 8 21 eclipsing binaries in SMC Hilditch+ 05, De Mink+ 07 Porbit= 1.1 days Porbit= 2 days Porbit= 3 days

    7. Why using binaries

    accurate masses + orbital period + filling factor (=R*/Rrl) -> direct comparison to model -> just a few well determined systems needed spin period = orbital period -> no sin(i) effect -> more accurate than v_rot from spectra history known -> no mass transfer / mergers surface abundances ? -> even just upper limits help extra mixing due to presence of companion ? ?

    8. Very Massive Binaries

    Rapid rotators ? Tight binaries

    9. Cartoon

    ? Bifurcation: Maeder 87, Yoon+05 Slow rotators

    10. Very Massive Binaries

    11. HRD: 50+25Msun LMC

    Normal evolution Stars stay compact De Mink & Cantiello + (in prep.)? [L72] LH 54-425: Williams+08, R136-38 Massey+02

    12. Surface Helium

    De Mink & Cantiello + (in prep.)? Normal evolution Quasi chemically homogeneous ‘’WR stars in disguise’’ ?

    13. Conclusion

    Eclipsing binaries as test for rotational mixing Predictions: Massive binaries -> Significant N enhancement Very massive binaries -> “Homogeneous evolution” New evolution channel for close WR binaries? surface abundances (or upperlimits) for detached, massive, close, eclipsing binaries

    14. Thank you

    Related posters: De Mink, S.E., Cantiello, M., et al. “Rotational mixing and massive binaries” Brott, I., Hunter, I., et al. “Constraints on rotational mixing from Magellanic clouds B stars ”

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