10.5281/zenodo.3406320
https://zenodo.org/records/3406320
oai:zenodo.org:3406320
Renzo, M.
M.
Renzo
0000-0002-6718-9472
University of Amsterdam - API
Farmer, R.
R.
Farmer
0000-0003-3441-7624
University of Amsterdam, API
Justham, S.
S.
Justham
0000-0001-7969-1569
Chinese accademy of Science
de Mink,. S. E.
. S. E.
de Mink
0000-0001-9336-2825
Harvard, CfA
Gotberg, Y.
Y.
Gotberg
0000-0002-6960-6911
The observatories of the Carnegie institution
Marchant, P.
P.
Marchant
0000-0002-0338-8181
KU Leuven
Sensitivity of the lower-edge of the pair instability black hole mass gap to the treatment of time dependent convection
Zenodo
2019
Massive stars
pulsational pair instability
supernovae
black holes
stellar convection
2019-09-12
eng
10.5281/zenodo.3406319
https://zenodo.org/communities/astronomy-general
https://zenodo.org/communities/api
Creative Commons Attribution 4.0 International
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]
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.
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.