@Article{KamlahLSAABBGHBKW:2022:EvSiBi,
               author = "Kamlah, A. W. H. and Leveque, A. and Spurzem, R. and Arca Sedda, 
                         M. and Askar, A. and Banerjee, S. and Berczik, P. and Giersz, M. 
                         and Hurley, J. and Belloni, Diogo Teixeira and K{\"u}hmichel, L. 
                         and Wang, L.",
          affiliation = "{Max-Planck-Institut f{\"u}r Astronomie} and {Peking University} 
                         and {University of Heidelberg} and {University of Heidelberg} and 
                         {Chinese Academy of Sciences} and {Polish Academy of Sciences} and 
                         {National Academy of Sciences of Ukraine} and {Peking University} 
                         and {Swinburne University of Technology} and {Instituto Nacional 
                         de Pesquisas Espaciais (INPE)} and {University of Heidelberg} and 
                         {The University of Tokyo}",
                title = "Preparing the next gravitational million-body simulations: 
                         evolution of single and binary stars in nbody6++gpu, mocca, and 
                         mcluster",
              journal = "Monthly Notices of the Royal Astronomical Society",
                 year = "2022",
               volume = "511",
               number = "3",
                pages = "4060--4089",
                month = "Feb.",
             keywords = "methods: numerical, software: development, software: 
                         documentation, binaries: general, stars: general, globular 
                         clusters: general.",
             abstract = "We present the implementation of updated stellar evolution recipes 
                         in the codes nbody6++gpu, mocca, and mcluster. We test them 
                         through numerical simulations of star clusters containing 1.1 x 
                         10(5) stars (with 2.0 x 10(4) in primordial hard binaries) 
                         performing high-resolution direct N-body (nbody6++gpu) and Monte 
                         Carlo (mocca) simulations to an age of 10 Gyr. We compare models 
                         implementing either delayed or core-collapse supernovae 
                         mechanisms, a different mass ratio distribution for binaries, and 
                         white dwarf (WD) natal kicks enabled/disabled. Compared to 
                         nbody6++gpu, the mocca models appear to be denser, with a larger 
                         scatter in the remnant masses, and a lower binary fraction on 
                         average. The mocca models produce more black holes (BHs) and 
                         helium WDs, while nbody6++gpu models are characterized by a much 
                         larger amount of WD-WD binaries. The remnant kick velocity and 
                         escape speed distributions are similar for the BHs and neutron 
                         stars (NSs), and some NSs formed via electron-capture supernovae, 
                         accretion-induced collapse, or merger-induced collapse escape the 
                         cluster in all simulations. The escape speed distributions for the 
                         WDs, on the other hand, are very dissimilar. We categorize the 
                         stellar evolution recipes available in nbody6++gpu into four 
                         levels: the one implemented in previous nbody6++gpu and mocca 
                         versions (level A), state-of-the-art prescriptions (level B), some 
                         in a testing phase (level C), and those that will be added in 
                         future versions of our codes.",
                  doi = "10.1093/mnras/stab3748",
                  url = "http://dx.doi.org/10.1093/mnras/stab3748",
                 issn = "0035-8711 and 1365-2966",
             language = "en",
           targetfile = "khamla_2022_preparing.pdf",
        urlaccessdate = "12 maio 2024"
}