The Geneva stellar evolution code

By P. Eggenberger, G. Meynet, Andre Maeder, R. Hirschi, C. Charbonnel, Suzanne Talon, S. Ekström. 2008

208 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ccceeb6d0d583f3940eea8747e07c9e75553226c

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Michela Mapelli
2. Stan Woosley
3. N. Langer
4. R. Hirschi
5. Aaron Dotter
6. C. Conroy
7. G. Meynet
8. D. Holz

Citations in the corpus

• Non-standard s process in low metallicity massive rotating stars (2011, methodology): “We calculated our models with the Geneva stellar evolution code (GENEC), which is described in detail in (Eggenberger et al., 2008).”
• Seismic diagnostics for transport of angular momentum in stars. I. Rotational splittings from the pre-main sequence to the red-giant branch. (2012, methodology): “Several stellar evolutionary codes already include transport of angular momentum and associated chemical element mixing (Chaboyer et al. 1995; Eggenberger et al. 2008; Palacios et al. 2003; Talon et al. 1997).”
• s-process production in rotating massive stars at solar and low metallicities (2015, methodology): “We calculated the stellar evolution models with the Geneva stellar evolution code (GENEC), which is described in detail in Eggenberger et al. (2008).”
• The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M⊙ stellar mass limit (2010, methodology): “Although a detailed description is provided elsewhere (Hirschi, Meynet & Maeder 2004), together with recent updates (Eggenberger et al. 2008), models include the physics of rotation and mass loss, which are both crucial to model the evolution of very massive stars.”
• NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, methodology): “The GENEC code (Eggenberger et al. 2008; Bennett et al. 2012; Pignatari et al. 2013) was used for massive stars.”
• Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes (2017, methodology): “Geneva stellar models The physics included in the employed Geneva rotating models are described in detail in Eggenberger et al. (2008), Ekström et al. (2012).”
• MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): PLANETS, OSCILLATIONS, ROTATION, AND MASSIVE STARS (2013, background): “This is a very common assumption in stellar evolution codes (e.g. Pinsonneault et al. 1989; Heger et al. 2000; Eggenberger et al. 2008); note however that helioseismology has clearly shown this is not the case for the solar convection zone (e.g. Brown et al. 1989; Thompson et al. 1996; Schou et al.…”
• MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, methodology): “All rotating models are initialized with solid body rotation on the zero age main sequence (ZAMS), which is the standard choice in stellar evolution codes (Pinsonneault et al. 1989; Heger et al. 2000; Eggenberger et al. 2008).”
• The mass-loss rates of red supergiants and the de Jager prescription (2010, methodology): “The dJ88 law was also used in past evolution models of the Geneva group (described in, e.g., Maeder & Meynet 1989; Eggenberger et al. 2008).”
• MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA) (2010, background): “For example, the participants (Christensen-Dalsgaard 2008; Degl’Innocenti et al. 2008; Demarque et al. 2008; Eggenberger et al. 2008; Hui-Bon-Hoa 2008; Morel & Lebreton 2008; Roxburgh 2008; Scuflaire et al. 2008; Ventura et al. 2008; Weiss & Schlattl 2008) in the CoRot Evolution and Seismic Tools…”
• Angular momentum transport in stellar interiors constrained by rotational splittings of mixed modes in red giants (2012, methodology): “We use the Geneva stellar evolution code that includes a detailed treatment of shellular rotation (Eggenberger et al. 2008).”
• Evolution and fate of very massive stars (2013, methodology): “…in groups, similarly to present-day star formation (Greif et al. 2010; Stacy, Greif & Bromm 2010). metallicities using the GENEVA stellar evolution code (Eggenberger et al. 2008) including the modifications implemented to follow the advanced stages as described in Hirschi, Meynet & Maeder (2004).”