Population synthesis of binary carbon-enhanced metal-poor stars

By Robert G. Izzard, E. Glebbeek, R. Stancliffe, Onno Pols Sterrenkundig Instituut, Universiteit Utrecht Institut d'Astronomie et d'Astrophysique, Universite de Montreal Department of Physics, Astronomy, MD Department of Astronomy, U. Sciences, M. University. 2009

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The carbon-enhanced metal-poor (CEMP) stars constitute approximately one fifth of the metal-poor ([Fe/H]

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/f6557680eaf03aad0b56aa764ac404f3cdb364b9

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Citations in the corpus

The s-Process in Low Metallicity Stars. II. Interpretation of High-Resolution Spectroscopic Observations with AGB models (2011, background): “The need of stars with low initial mass has also been invoked by Izzard et al. (2009) to explain the high fraction of carbon enhanced stars among very metalpoor stars.”
Binarity in carbon-enhanced metal-poor stars (2014, background): “Each individual probability,p(fbin, Pmax|D,M), is subsequently normalized by the sum of all probabilities across our model parameters.”
Re-evaluating old stellar populations (2018, methodology): “MNRAS 000, 1–17 (2018) Here the rapid population synthesis approach used in codes such as binary c (Izzard et al. 2009; Abate et al. 2015), in which analytic prescriptions and empirical relations are used to infer the population, or in which interpolation occurs between a much coarser model grid,…”
THE ROTATION RATES OF MASSIVE STARS: THE ROLE OF BINARY INTERACTION THROUGH TIDES, MASS TRANSFER, AND MERGERS (2012, methodology): “In addition it allows us to explore the effects of uncertain parameters (cf. Izzard et al. 2009).”
COSMIC Variance in Binary Population Synthesis (2019, background): “…(Hurley et al. 2002), SeBa (Portegies Zwart & Verbunt 1996; Nelemans et al. 2001; Toonen et al. 2012), StarTrack (Belczynski et al. 2002, 2008), binary c (Izzard et al. 2004, 2006, 2009), COMPAS (Stevenson et al. 2017; Barrett et al. 2018), and MOBSE (Giacobbo et al. 2018; Giacobbo & Mapelli 2018).”
Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results (2017, background): “…are several codes and groups that study and account for interacting binaries in population synthesis (e.g. Belczynski et al. 2008; De Donder & Vanbeveren 2004; Hurley, Tout, & Pols 2002; Izzard et al. 2009; Lipunov et al. 2009; Toonen & Nelemans 2013; Tutukov & Yungelson 1996; Willems & Kolb 2004).”
THE INCIDENCE OF STELLAR MERGERS AND MASS GAINERS AMONG MASSIVE STARS (2013, methodology): “This code was originally developed by Hurley et al. (2000, 2002) and Izzard et al. (2004, 2006, 2009) based on stellar models by Pols et al. (1998).”
Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction (2017, methodology): “We use a binary population synthesis code, binary_c (version 2.0, SVN revision 4105), developed by Izzard et al. (2004, 2006, 2009) with updates described in de Mink et al. (2013) and Schneider et al. (2015).”
The evolution of isotope ratios in the Milky Way Galaxy (2011, background): “A significant fraction of metal-poor stars show carbon en- richment (CEMP stars), with several scenarios proposed to explain the observed abundances including a single supernova (e.g., Umeda & Nomoto 2002) and AGB stars in binary systems (Suda et al. 2004; Lugaro et al. 2008; Izzard et al. 2009).”
Dawes Review 6: The Impact of Companions on Stellar Evolution (2016, methodology): “The BINARY_C code (Izzard et al., 2004, 2006, 2009), adds nucleosynthesis, updated physics, a suite of software for population synthesis and visualisation, and an API (Application Programming Interface).”
CARBON-ENHANCED METAL-POOR STARS IN SDSS/SEGUE. I. CARBON ABUNDANCE ESTIMATION AND FREQUENCY OF CEMP STARS (2013, methodology): “However, Izzard et al. (2009) and Abate et al. (2013), using a binary population model alone, could not reproduce the high fraction of CEMP stars among the most metal-poor stars.”
Massive runaway and walkaway stars (2018, methodology): “We carry out population synthesis calculations of isolated binaries with the rapid binary evolution code binary_c (Izzard et al. 2004b, 2006, 2009, 2018; de Mink et al. 2013; Schneider et al. 2015).”
Theoretical uncertainties of the Type Ia supernova rate (2014, methodology): “We employ the rapid binary evolution codebinary c/nucsyn based on the work of Hurley et al. (2000, 2002) with updates described in Izzard et al. (2004, 2006, 2009) and below.”
Merging black hole binaries with the SEVN code (2018, background): “…including SEBA (Portegies Zwart & Verbunt 1996; Toonen, Nelemans & Portegies Zwart 2012; Mapelli et al. 2013; Schneider et al. 2017), BINARY C (Izzard et al. 2004, 2006, 2009), STARTRACK (Belczynski et al. 2008, 2010, 2016a) and COMPAS (Barrett et al. 2017; Stevenson, Berry & Mandel 2017).”
Wind Roche-lobe overflow: Application to carbon-enhanced metal-poor stars (2013, methodology): “In order to perform this study we make use of the binary population synthesis code described by Izzard et al. (2004, 2006, 2009).”
Progenitors of gravitational wave mergers: binary evolution with the stellar grid-based code ComBinE (2018, methodology): “…synthesis studies performed with the codes StarTrack (Belczynski et al. 2008; Dominik et al. 2013, 2015; Chruslinska et al. 2018), binary c (Izzard et al. 2004, 2006, 2009, 2018), BPASS (Eldridge & Stanway 2016; Eldridge et al. 2017), COMPAS (Stevenson et al. 2017a; Barrett et al. 2017;…”