PRE-SUPERNOVA EVOLUTION OF ROTATING SOLAR METALLICITY STARS IN THE MASS RANGE 13–120 M☉ AND THEIR EXPLOSIVE YIELDS

By A. Chieffi, M. Limongi. 2012

211 citations recorded by the source corpus.

We present the first set of a new generation of models of massive stars with a solar composition extending between 13 and 120 M☉, computed with and without the effects of rotation. We included two instabilities induced by rotation: the meridional circulation and the shear instability. We implemented two alternative schemes to treat the transport of the angular momentum: the advection–diffusion formalism and the simpler purely diffusive one. The full evolution from the pre-main sequence up to the pre-supernova stage is followed in detail with a very extended nuclear network. The explosive yields are provided for a variety of possible mass cuts and are available at the Web site http://www.iasf-roma.inaf.it/orfeo/public_html. We find that both the He and the CO core masses are larger than those of their non-rotating counterparts. Also the C abundance left by the He burning is lower than in the non-rotating case, especially for stars with an initial mass of 13–25 M☉, and this affects the final mass–radius relation, basically the final binding energy, at the pre-supernova stage. The elemental yields produced by a generation of stars rotating initially at 300 km s−1 do not change substantially with respect to those produced by a generation of non-rotating massive stars, the main differences being a slight overproduction of the weak s-component and a larger production of F. Since rotation also affects the mass-loss rate, either directly or indirectly, we find substantial differences in the lifetimes as O-type and Wolf–Rayet subtypes between the rotating and non-rotating models. The maximum mass exploding as Type IIP supernova ranges between 15 and 20 M☉ in both sets of models (this value depends basically on the larger mass-loss rates in the red supergiant phase due to the inclusion of the dust-driven wind). This limiting value is in remarkably good agreement with current estimates.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/b2bcb9e0e8e9a6eaf28e13d088cc5d46f8c1efb3

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In Astronomy and Astrophysics

1. R. Hirschi
2. G. Meynet
3. M. Limongi
4. A. Chieffi
5. C. Conroy
6. Stan Woosley
7. Michela Mapelli
8. S. Ekström

Citations in the corpus

• s-process production in rotating massive stars at solar and low metallicities (2015, result): “In particular, they have more massive helium burning and CO-cores (see Table 2), respectively, which is an effect of rotation also found by other studies (e.g. Heger & Langer 2000; Chieffi & Limongi 2013).”
• The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, unknown): “…configuration of convective burning shells at collapse varies tremendously across different progenitors in 1D stellar evolution models as, e.g., the Kippenhahn diagrams in the literature indicate (Heger et al. 2000; Chieffi & Limongi 2013; Sukhbold & Woosley 2014; Cristini et al. 2016) indicate.”
• PREPARING FOR AN EXPLOSION: HYDRODYNAMIC INSTABILITIES AND TURBULENCE IN PRESUPERNOVAE (2013, background): “…is not yet good detailed agreement in the final stellar structure among the various evolution groups (see Georgy, Ekström, Meynet, et al. (2012), Chieffi & Limongi (2013), Bill Paxton, private communication), even though they all use some version of MLT (this may be related to differing mixing…”
• THE EFFECTS OF STELLAR ROTATION. II. A COMPREHENSIVE SET OF STARBURST99 MODELS (2014, background): “Chieffi & Limongi (2013) also released models for the pre-supernova evolution of rotating solar metallicity stars.”
• Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements (2018, methodology): “As already discussed extensively in Chieffi & Limongi (2013) and references therein, the efficiency of the rotation driven mixing cannot be determined on the basis of first principles because, similarly to what happens for the thermal instabilities (convection), it is intrinsically a…”
• Exploring Fundamentally Three-dimensional Phenomena in High-fidelity Simulations of Core-collapse Supernovae (2018, background): “…is typically silicon shell that is undergoing nuclear burning that may or may not be convective at the point of core collapse, depending on the preceding evolution (cf., Chieffi & Limongi 2013; Sukhbold & Woosley 2014), above this silicon shell is an oxygen shell that is also typically convective.”
• The cosmic merger rate of stellar black hole binaries from the Illustris simulation (2017, methodology): “…that we keep using the original fitting formulas of Hurley et al. (2000) for the photospheric radius and luminosity of stars, while our knowledge of the evolution of massive stars changed significantly in the last decades (e.g. Martins & Palacios 2013; Chieffi & Limongi 2013; Chen et al. 2015).”
• MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “…1997; Heger et al. 2000; Maeder & Meynet 2000; Palacios et al. 2003; Talon & Charbonnel 2005; Denissenkov & Pinsonneault 2007; Hunter et al. 2007; Chieffi & Limongi 2013; Cantiello et al. 2014), but it remains as one of the most challenging and uncertain problems in stellar astrophysics.”
• Evolution and fate of very massive stars (2013, background): “…al. (2012, and references therein), the large angular momentum content is most interesting for the stars that just fall short of the minimum CO core mass for PCSN (since fast rotation plays an important role during the early collapse; Ott et al. 2004; O’Connor & Ott 2011; Chieffi & Limongi 2013).”