================================================================================ 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. ================================================================================

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).