A new synthetic model for asymptotic giant branch stars

By Robert G. Izzard, C. Tout, A. Karakas, O. Pols. 2004

230 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1b56045973c65cd52045a5cfddc161420a566276

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Citations in the corpus

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).”
Evolution of Asymptotic Giant Branch Stars (2005, methodology): “Other sets of synthetic models have been constructed with specific applications in mind, including synthetic binary models (Izzard et al. 2004) or old- and intermediate-age populations as tools to study extra-galactic systems (Mouhcine & Lançon 2002).”
Evolution of asymptotic giant branch stars. II. Optical to far-infrared isochrones with improved TP- (2007, background): “The invariance of O is a common assumption, since standard predictions of detailed AGB nucleosynthesis indicate that the material dredged-up at thermal pulses comprises only a small amount of oxygen, i.e.XO ∼ 0.5− 4% (Boothroyd & Sackmann 1988; Izzard et al. 2004).”
Evolution of asymptotic giant branch stars. I. Updated synthetic TP-AGB models and their basic calibration (2007, background): “Only very recently extended grids of complete AGB models have become available (e.g., K02; I04), allowing us to relax the crude simplification of constant Mminc in place of a more physically sound dependence on stellar mass and metallicity.”
Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results (2017, methodology): “In future, we will recalculate these models with realistic AGB massloss rates to terminate the evolution earlier or add a routine with in the population synthesis to use rapid synthetic model of AGB evolution (e.g. Izzard et al. 2004).”
Constraining the thermally pulsing asymptotic giant branch phase with resolved stellar populations in the Large Magellanic Cloud (2019, unknown): “…was later revised with increasingly detailed models of the AGB evolution (e.g. Marigo, Girardi & Bressan 1999; Marigo, Girardi & Chiosi 2003; Izzard et al. 2004; Stancliffe, Izzard & Tout 2005; Marigo et al. 2013, 2017), and extended to many dwarf galaxies with good estimates of their star…”
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.”
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).”
Origin of multiple stellar populations in globular clusters and their helium enrichment (2008, methodology): “In this respect, the schematic AGB evolution adopted here differs from AGB models existing in the literature (e.g. Renzini & Voli 1981; Groenewegen & de Jong 1993; Herwig 2004; Izzard et al. 2004; Ventura & D’Antona 2005, 2008; Marigo & Girardi 2007).”
Post-common-envelope binaries from SDSS. IX: Constraining the common-envelope efficiency (2010, unknown): “(29) in Izzard et al. (2004).”
Predicting the LISA white dwarf binary population in the Milky Way with cosmological simulations (2019, background): “Chemical enrichment stems from type Ia supernovae (Iwamoto et al. 1999), core-collapse supernovae (Nomoto et al. 2006), and O and AGB star winds (van den Hoek & Groenewegen 1997; Marigo 2001; Izzard et al. 2004).”
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).”
STELLAR YIELDS FROM METAL-RICH ASYMPTOTIC GIANT BRANCH MODELS (2016, methodology): “A fine grid of masses is required in order to provide accurate yield predictions for Galactic chemical evolution models, as discussed by Izzard et al. (2004) in the context of synthetic, rapid AGB models.”
FIRE-2 simulations: physics versus numerics in galaxy formation (2017, methodology): “Yields for OB/AGB winds are taken from the synthesis of the models from van den Hoek & Groenewegen (1997), Marigo (2001), and Izzard et al. (2004) as synthesized in Wiersma et al. (2009b), appropriately re-averaged over the IMF.”
The structure and dynamical evolution of the stellar disc of a simulated Milky Way-mass galaxy (2016, methodology): “We follow Wiersma et al. (2009b) and account for metal production from Type-II SNe, Type-Ia SNe, and stellar winds using the metal yields in Woosley & Weaver (1995), Iwamoto et al. (1999), and Izzard et al. (2004), respectively.”
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).”
Quantifying the uncertainties of chemical evolution studies II. Stellar yields (2010, result): “The latter, for instance, is the case of the yields presented by Izzard et al. (2004), which are very similar to the ones by Karakas & Lattanzio (2007) (see figures from 2 to 7 of Karakas & Lattanzio 2007) and are thus not included in the present study.”
EVOLUTION, NUCLEOSYNTHESIS, AND YIELDS OF LOW-MASS ASYMPTOTIC GIANT BRANCH STARS AT DIFFERENT METALLICITIES (2009, background): “Notwithstanding, Izzard et al. (2004) concluded that full stellar evolutionary models cannot reproduce the Magellanic Clouds LFCS, being the evolutionary models too luminous with respect to the observed distributions.”