Renzo, M.
Farmer, R.
Justham, S.
de Mink,. S. E.
Gotberg, Y.
Marchant, P.
2019-09-12
<p>Numerical results of the simulations presented in Monthly Notices of the Royal Astronomical Society, Volume 493, Issue 3, p.4333-4341 [https://ui.adsabs.harvard.edu/abs/2020MNRAS.493.4333R/abstract]<br>
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Models are named as string_MASS.tar.xz, where MASS is the initial He core mass in solar mass units, and string is either "classic_MLT" for the models computed with MESA 10108, "timedependentdecel" for models computed with MESA 11123 using the time dependent convection treatment from Marchant et al. 2018, "timedependentdecel_no_undershooting" for those computed without undershooting, and "timedependentdecel_high_semiconv" for those computed assuming a semiconvection efficiency of 0.1 (instead of 0.01). The template_string.tar.xz contain the input files necessary to reproduce our results with the corresponding MESA version listed above.</p>
<p> </p>
<p><br>
Each tarball contains the history file, a few MESA profile saved at specific evolutionary phases (before turning on the hydro in MESA at each pulse and at the onset of core-collapse), and the input files to reproduce them. We also provide template input files at mesastar.org.</p>
https://doi.org/10.5281/zenodo.3406320
oai:zenodo.org:3406320
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https://doi.org/10.5281/zenodo.3406319
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Massive stars
pulsational pair instability
supernovae
black holes
stellar convection
Sensitivity of the lower-edge of the pair instability black hole mass gap to the treatment of time dependent convection
info:eu-repo/semantics/article