Massive Stars in the Range 13-25 M⊙: Evolution and Nucleosynthesis. II. The Solar Metallicity Models

By M. Limongi, O. Straniero, A. Chieffi. 2000

136 citations recorded by the source corpus.

We present the evolutionary properties of a set of massive stellar models (namely 13, 15, 20, and 25 M⊙) from the main-sequence phase up to the onset of the iron core collapse. All these models have initial solar chemical composition, i.e., Y = 0.285 and Z = 0.02. A 179 isotope network, extending from neutron up to 68Zn and fully coupled to the evolutionary code has been adopted from the carbon burning onward. Our results are compared, whenever possible, to similar computations available in literature.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/8f0ccc64068d757aa5dbd497460d23cf855a0407

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

Citations in the corpus

s-process production in rotating massive stars at solar and low metallicities (2015, background): “Other neutron sources as 17O(α, n) and 21Ne(α, n) recycle most of the MNRAS 456, 1803–1825 (2016) at K eele U niversity on N ovem ber 23, 2016 http://m nras.oxfordjournals.org/ D ow nloaded from neutrons absorbed by 16O and 20Ne, respectively (e.g. Limongi et al. 2000).”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, methodology): “…et al. (1973); Arnett & Thielemann (1985); Thielemann & Arnett (1985); Woosley & Weaver (1995); Thielemann et al. (1996); Chieffi et al. (1998); Limongi et al. (2000); Rauscher et al. (2002); Woosley et al. (2002) for similar analysis and discussion but focused only on massive stars, while we…”
Explosive Yields of Massive Stars from Z = 0 to Z = Z☉ (2004, background): “Some years ago we began a long-term project devoted to the study of the evolution of massive stars and their associated explosive yields (Chieffi et al. 1998; Limongi et al. 2000; Limongi & Chieffi 2002, 2003, hereafter LC03; Chieffi & Limongi 2002).”
Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements (2018, background): “…of yields from massive stars (hereafter MS) for an extensive grid of isotopes (H to Zn), stellar masses and metallicities (Woosley & Weaver 1995; Limongi et al. 2000; Chieffi & Limongi 2004; Limongi & Chieffi 2012; Chieffi & Limongi 2013; Umeda & Nomoto 2002; Nomoto et al. 2006; Heger & Woosley…”
Nucleosynthesis in Massive Stars with Improved Nuclear and Stellar Physics (2001, background): “Most recently, nucleosynthesis in massive stars has been studied by Woosley & Weaver (1995, WW95); Thielemann et al. (1996); Limongi et al. (2000) and others.”
Three-dimensional simulations of core-collapse supernovae: from shock revival to shock breakout (2014, methodology): “W15 denotes the 15 M RSG model s15s7b2 of Woosley & Weaver (1995), L15 a 15 M RSG model evolved by Limongi et al. (2000), N20 a 20 M BSG progenitor model for SN 1987A by Shigeyama & Nomoto (1990), and B15 a corresponding 15 M BSG model by Woosley et al. (1988).”
Three-dimensional neutrino-driven supernovae: neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products (2012, background): “W15 is based on the nonrotating 15 M model s15s7b2 of Woosley & Weaver (1995), L15 corresponds to a star evolved by Limongi et al. (2000), B15 is a blue supergiant (SN 1987A) progenitor of Woosley et al. (1988), and N20 was computed up to core collapse by Shigeyama & Nomoto (1990).”
The s process: Nuclear physics, stellar models, and observations (2010, methodology): “…by post-process models and full stellar models describing the evolution of massive stars up to the final burning phases and the SN explosion (El Eid et al., 2009; Limongi et al., 2000; Pignatari et al., 2010; Raiteri et al., 1993; The et al., 2007; Woosley et al., 2002; Woosley and Weaver, 1995).”
Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport II. Models for different progenitor stars (2005, background): “Only in case of the progenitors from Limongi et al. (2000) the prompt shock pushes out a bit farther.”
Evolution of Stars and Stellar Populations (2005, methodology): “the silicon burning stage as given by [130].”
Reconstructing the star formation history of the Milky Way disc(s) from chemical abundances (2014, unknown): “For example, Chiappini et al. (1997) use Woosley & Weaver (1995) yields while Fenner & Gibson (2003) use Limongi et al. (2000); Limongi & Chieffi (2002) yields etc.”
Stellar evolution with rotation XII. Pre-supernova models (2004, methodology): “At the same time, recent non–rotating 13 M⊙ models in Woosley et al. (2002) and Limongi et al. (2000) reach core–collapse.”