Black hole masses at solar metallicity are set by whether a star becomes a Wolf-Rayet star before collapse, and cool supergiant winds control that split.
The dependence of convective core overshooting on stellar mass: Additional binary systems and improved calibration
4 Pith papers cite this work. Polarity classification is still indexing.
4
Pith papers citing it
abstract
Many current stellar evolution models assume some dependence of the strength of convective core overshooting on mass for stars more massive than 1.1-1.2 solar masses, but the adopted shapes for that relation have remained somewhat arbitrary for lack of strong observational constraints. In previous work we compared stellar evolution models to well-measured eclipsing binaries to show that, when overshooting is implemented as a diffusive process, the fitted free parameter f(ov) rises sharply up to about 2 solar masses, and remains largely constant thereafter. Here we analyze a new sample of eight binaries selected to be in the critical mass range below 2 solar masses where f(ov) is changing the most, nearly doubling the number of individual stars in this regime. This interval is important because the precise way in which f(ov) changes determines the shape of isochrones in the turnoff region of 1-5 Gyr clusters, and can thus affect their inferred ages. It also has a significant influence on estimates of stellar properties for exoplanet hosts, on stellar population synthesis, and on the detailed modeling of interior stellar structures, including the calculation of oscillation frequencies that are observable with asteroseismic techniques. We find that the derived f(ov) values for our new sample are consistent with the trend defined by our earlier determinations, and strengthen the relation. This provides an opportunity for future series of models to test the new prescription, grounded on observations, against independent observations that may constrain overshooting in a different way.
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astro-ph.SR 4years
2026 4representative citing papers
The primary star in the detached eclipsing binary V0757 Pup is a gamma Doradus pulsator with persistent frequencies near 0.79 and 0.98 cycles per day.
Binary evolution modeling constrains donor masses of 14-23 solar masses for two luminous red novae and shows dust masses are 1-5 orders of magnitude below total ejected envelope masses.
MESA models show residual hydrogen envelope mass sets effective temperature on the horizontal branch, with maximum values of 0.05-0.30 solar masses to avoid later thermally pulsing AGB evolution, plus explanations for blue hook stars and puffed-up pre-HB configurations.
citing papers explorer
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The Stellar Winds Atlas II: Black Hole Formation at Solar Metallicity
Black hole masses at solar metallicity are set by whether a star becomes a Wolf-Rayet star before collapse, and cool supergiant winds control that split.
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First and Comprehensive Study of V0757 Pup : $\gamma-$Doradus Pulsator in Detached Eclipsing Binary
The primary star in the detached eclipsing binary V0757 Pup is a gamma Doradus pulsator with persistent frequencies near 0.79 and 0.98 cycles per day.
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Comparative Study of Two Luminous Red Novae I. Progenitor Modeling and Dust Formation
Binary evolution modeling constrains donor masses of 14-23 solar masses for two luminous red novae and shows dust masses are 1-5 orders of magnitude below total ejected envelope masses.
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Shaping the horizontal branch: The role of envelope mass in the evolution of stripped core-helium-burning stars
MESA models show residual hydrogen envelope mass sets effective temperature on the horizontal branch, with maximum values of 0.05-0.30 solar masses to avoid later thermally pulsing AGB evolution, plus explanations for blue hook stars and puffed-up pre-HB configurations.