Ben Hastings

TL;DR: In this article, the authors analyzed a large grid of detailed binary evolution models at LMC metallicity with initial primary masses between 10 and 40 M, and identified the model systems that potentially evolve into a binary consisting of a black hole and a massive main-sequence star.

TL;DR: In this paper, the authors used a dense model grid of more than 50,000 detailed binary-evolution calculations to show several distinct, coeval main-sequence (MS) components, most notably an extended MS turnoff region, and a group of nearcritical rotating stars that is spread over a large luminosity range on the red side of the classical MS.

TL;DR: In this paper, the authors analyzed a large grid of detailed binary evolution models at LMC metallicity with initial primary masses between 10 and 40 Msun, and identified which model systems potentially evolve into a binary consisting of a black hole and a massive main sequence star.

TL;DR: In this article, the authors identify the main effects which are responsible for single stars to approach critical rotation as functions of initial mass and metallicity, and predict the properties of populations of rotating single stars.

TL;DR: In this article, the authors used a large grid of ~10,000 detailed binary evolution models calculated with the stellar evolution code MESA, covering initial donor masses between 10-40 M$_{\odot}$ and initial orbital periods above 1.4 d, at a metallicity suitable for the Large Magellanic Cloud (LMC).