Evolution of Asymptotic Giant Branch Stars

By Falk Herwig. 2005

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In Astronomy and Astrophysics

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EVOLUTION, NUCLEOSYNTHESIS, AND YIELDS OF AGB STARS AT DIFFERENT METALLICITIES. III. INTERMEDIATE-MASS MODELS, REVISED LOW-MASS MODELS, AND THE pH-FRUITY INTERFACE (2015, background): “The interested reader can find a vast literature on AGB stars (Iben & Renzini 1983; Herwig 2005; Straniero et al. 2006; Karakas & Lattanzio 2014).”
Neutron-Capture Elements in the Early Galaxy (2008, background): “(See the reviews by Busso, Gallino & Wasserburg 1999; Straniero et al. 2003; Busso et al. 2004; Herwig 2005; Straniero, Gallino & Cristallo 2006.)”
CHEMICAL ABUNDANCES FOR 855 GIANTS IN THE GLOBULAR CLUSTER OMEGA CENTAURI (NGC 5139) (2010, background): “…the s–process is widely believed to be active in thermally pulsing low and intermediate mass AGB stars, but theoretical models indicate that most of the s–process element production is probably constrained to stars in the range ∼1.3–3 M (e.g., Busso et al. 1999; Herwig 2005; Straniero et al. 2006).”
Evolution of asymptotic giant branch stars. I. Updated synthetic TP-AGB models and their basic calibration (2007, background): “…facts such as the conversion from M to C spectral types in AGB stars with initial masses and luminosities as low as Appendix A is only available in electronic form at http://www.aanda.org Mi ∼ 1.5 M and Mbol ∼ −3.5 (see Herwig 2005, for a review; and Stancliffe et al. 2005, for a recent exception).”
Evolution of massive AGB stars - II. model properties at non-solar metallicity and the fate of Super-AGB stars (2007, background): “In the abundant literature on AGB stars (Herwig 2005), the characteristics of 3DUP (time of occurrence, depth, long term evolution) are still debated and are sensitive to numerical factors such as spatial resolution (Straniero et al. 1997), interpolation of constitutive variables (Pols & Tout…”
CARBON-ENHANCED METAL-POOR STARS IN SDSS/SEGUE. I. CARBON ABUNDANCE ESTIMATION AND FREQUENCY OF CEMP STARS (2013, background): “…envelope of an asymptotic giant 15 [C/Fe]=log10(N(C) /N(Fe))⋆ – log10(N(C)/N(Fe))⊙ branch (AGB) star to its (presently observed) binary companion (e.g., Herwig 2005; Sneden et al. 2008; Masseron et al. 2010; Bisterzo et al. 2011, 2012); (2) massive, rapidly rotating, zero-metallicity stars, which…”
The ATLAS3D Project – XXVIII. Dynamically driven star formation suppression in early-type galaxies (2014, background): “All stars between 0.8 and 8M⊙ will go through an AGB stage (Herwig 2005), but from a single burst of star formation the number of stars going through this (relatively short-lived) phase is a strong function of time.”
Constraining the thermally pulsing asymptotic giant branch phase with resolved stellar populations in the Large Magellanic Cloud (2019, background): “…(with initial masses in the range 0.8 M Mi 6 − 8 M ) experience helium and hydrogen double shell-burning, reach their highest luminosity, synthesize new chemical elements, undergo powerful mass-loss via stellar winds, and then finally reach the stage of white dwarfs (WDs; Herwig 2005).”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “The TPAGB phase is famous both for its namesake thermal pulses triggered by alternating hydrogen and helium burning in shells (see Section 8.5 for a more detailed explanation) and high mass loss rates (see Herwig 2005 for an excellent review).”
FORMATION OF FULLERENES IN H-CONTAINING PLANETARY NEBULAE (2010, background): “…are not expected to be formed in the hydrogenrich circumstellar envelopes of cool, evolved stars (e.g., C-rich asymptotic giant branch (AGB) stars; Herwig 2005) and in the interstellar medium (De Vries et al. 1993), in spite of the fact that C-rich AGB stars are the sites of a complex and rich…”
Pulsating white dwarfs: new insights (2019, background): “On the TP-AGB phase, stars undergo intense radiation dust-driven winds as high as Ṁ ∼ 10−4M⊙/yr, where most of the envelope can be removed in less than one million years, leaving a carbonoxygen (CO) core WD (Herwig, 2005; Höfner and Olofsson, 2018).”
CARBON-ENHANCED METAL-POOR STAR FREQUENCIES IN THE GALAXY: CORRECTIONS FOR THE EFFECT OF EVOLUTIONARY STATUS ON CARBON ABUNDANCES (2014, background): “This pattern is thought to be the result of mass transfer across a binary system, coming from an evolved star that has passed through the asymptotic giant branch (AGB; e.g., Herwig 2005) evolutionary stage.”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, background): “This choice is motivated by observational constraints, as for example the maximum level of C enhancement seen in Crich stars and planetary nebulae (Herwig 2005), as well as by recent hydrodynamics simulations investigating mass loss rates in C-rich giants (e.g., Mattsson et al. 2010; Mattsson &…”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA) (2010, background): “008 (Herwig 2005).”
The evolution of isotope ratios in the Milky Way Galaxy (2011, background): “This mixing is known as the third dredge-up (TDU), and is responsible for enriching the surface in 12C and other products of He-burning, as well as elements heavier than Fe produced by the slow neutron capture process (Busso Gallino; Herwig 2005).”