Published May 22, 2023 | Version v1
Software Open

Inlists for paper: ALUMINIUM-26 FROM MASSIVE BINARY STARS III. BINARY STARS UP TO CORE-COLLAPSE AND THEIR IMPACT ON THE EARLY SOLAR SYSTEM

Authors/Creators

  • 1. Institute of Astronomy, KU Leuven
  • 2. School of Physics and Astronomy, Monash University
  • 3. Konkoly Observatory CSFK MTA
  • 4. Department of Astrophysics, Radboud University

Description

================================================================================
Title: Aluminium-26 From Massive Binary Stars III: BINARY STARS UP TO CORE-COLLAPSE AND THEIR IMPACT ON THE EARLY SOLAR SYSTEM
Authors: Brinkman H.E., Doherty C.L., Pignatari M., Pols, O.R., Lugaro M.
================================================================================
Description of contents: A .tar.gz package containing the input files for the
 MESA simulations of massive (10 {<=} M*(solmass) {<=} 80) non-rotating,
 binary stars at solar metallicity (Z=0.014). The nuclear network
 used is also given, RadioSupernova.net

BINARY/ contains the inlists used for the binary systems. There are 4 basic files per star, as well as 3 files
controlling the binary settings. The "inlist" file is the master inlist that MESA reads when it starts.
The "inlist" file is the master inlist that MESA reads when it starts. It reads the "binary_job", "binary_controls", and
 "binary_pg" inlist files. "binary_job" refers to the individual inlist for the stars, which are labeled "1" for the
 primary and "2" for the secondary. These inlists are the same as for Paper II.
PRIMARY/ contains the inlists for the decoupled binary, and these are identical to the primary inlists and the inlists used
for Paper II.
The run_star_extras.f is given as well.

System requirements: The MESA stellar evolution code. Version 10398 was used
 for these input files.

Additional comments: See section 2 for full details of the simulations.

================================================================================

Notes

HEB, MP, and ML acknowledge the support from the ERC Consolidator Grant (Hungary) program (RADIOSTAR, G.A. n. 724560). HEB acknowledges support from the Research Foundation Flanders (FWO) under grant agreement G089422N. MP acknowledge the support to NuGrid from JINA-CEE (NSF Grant PHY-1430152) and STFC (through the University of Hull's Consolidated Grant ST/R000840/1), and ongoing access to {\tt viper}, the University of Hull High Performance Computing Facility. MP and ML acknowledge the "Lend{\"u}let-2014" Program of the Hungarian Academy of Sciences (Hungary) for support. This work was supported by the European Union's Horizon 2020 research and innovation program (ChETEC-INFRA -- Project no. 101008324), and the IReNA network supported by US NSF AccelNet (Grant No. OISE-1927130).

Files

Files (12.5 kB)

Name Size Download all
md5:923b6f246eb00ea575d6bed531b609c0
12.5 kB Download

Additional details

Funding

UK Research and Innovation
Astrophysics at The University of Hull ST/R000840/1
European Commission
RADIOSTAR - Radioactivities from Stars to Solar Systems 724560
U.S. National Science Foundation
JINA Center for the Evolution of the Elements 1430152
U.S. National Science Foundation
AccelNet-WOU: International Research Network for Nuclear Astrophysics (IReNA) 1927130
European Commission
ChETEC-INFRA - Chemical Elements as Tracers of the Evolution of the Cosmos - Infrastructures for Nuclear Astrophysics 101008324