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Massive star evolution revealed in the Mass-Luminosity plane

Published online by Cambridge University Press:  30 December 2019

Erin R. Higgins  and
Jorick S. Vink
Erin R. Higgins
Affiliation:
Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, N. Ireland Queen’s University of Belfast, Belfast BT7 1NN, N. Ireland Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin, Ireland Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA emails: eh@arm.ac.uk, jsv@arm.ac.uk
Jorick S. Vink
Affiliation:
Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, N. Ireland Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA emails: eh@arm.ac.uk, jsv@arm.ac.uk
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Abstract

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Massive star evolution is dominated by key physical processes such as mass loss, convection and rotation, yet these effects are poorly constrained, even on the main sequence. We utilise a detached, eclipsing binary HD166734 as a testbed for single star evolution to calibrate new MESA stellar evolution grids. We introduce a novel method of comparing theoretical models with observations in the ‘Mass-Luminosity Plane’, as an equivalent to the HRD (see Higgins & Vink 2018). We reproduce stellar parameters and abundances of HD166734 with enhanced overshooting (αov=0.5), mass loss and rotational mixing. When comparing the constraints of our testbed to the systematic grid of models we find that a higher value of αov=0.5 (rather than αov=0.1) results in a solution which is more likely to evolve to a neutron star than a black hole, due to a lower value of the compactness parameter.

Keywords

stars: mass lossstars: evolutionstars: rotationconvection
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 480 - 485
Copyright
© International Astronomical Union 2019 

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