Nucleosynthesis in Massive Stars with Improved Nuclear and Stellar Physics

By T. Rauscher, Alexander Heger, R. Hoffman, S. W. B. U. O. Basel, Switzerland., Ucsc, Usa, U. Chicago, Llnl. 2001

739 citations recorded by the source corpus.

We present the first calculations to follow the evolution of all stable nuclei and their radioactive progenitors in stellar models computed from the onset of central hydrogen burning through explosion as Type II supernovae. Calculations are performed for Population I stars of 15, 19, 20, 21, and 25 M☉ using the most recently available experimental and theoretical nuclear data, revised opacity tables, neutrino losses, and weak interaction rates and taking into account mass loss due to stellar winds. A novel "adaptive" reaction network is employed with a variable number of nuclei (adjusted each time step) ranging from ~700 on the main sequence to ≳2200 during the explosion. The network includes, at any given time, all relevant isotopes from hydrogen through polonium (Z = 84). Even the limited grid of stellar masses studied suggests that overall good agreement can be achieved with the solar abundances of nuclei between 16O and 90Zr. Interesting discrepancies are seen in the 20 M☉ model and (so far, only in that model) are a consequence of the merging of the oxygen, neon, and carbon shells about a day prior to core collapse. We find that, in some stars, most of the "p-process" nuclei can be produced in the convective oxygen-burning shell moments prior to collapse; in others, they are made only in the explosion. Serious deficiencies still exist in all cases for the p-process isotopes of Ru and Mo.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/4c0864f03bdfd011a6e342953fe8ecb7be566255

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Citations in the corpus

Nucleosynthesis in Early Supernova Winds. II. The Role of Neutrinos (2005, background): “However, since these same nuclei were already made by other processes (Woosley et al. 2002; Rauscher et al. 2002), there seemed to be no clear diagnostic of the proton-rich wind.”
Composition of the Innermost Core-Collapse Supernova Ejecta (2004, background): “Supernova nucleosynthesis predictions have a long tradition (Woosley & Weaver 1986; Thielemann et al. 1990; Woosley & Weaver 1995; Thielemann et al. 1996; Nomoto et al. 1997; Nakamura et al. 2001; Rauscher et al. 2002; Chieffi & Limongi 2002; Chieffi & Limongi 2004; Umeda & Nomoto 2005).”
NEUTRON-RICH CHROMIUM ISOTOPE ANOMALIES IN SUPERNOVA NANOPARTICLES (2010, methodology): “A 54Fe/56Fe ratio between ~0.01 and 0.7×solar can be produced in the O/Ne and O/C zones of type II supernovae (Rauscher et al. 2002; http://nucastro.org/nucleosynthesis/), which would reduce the 54Fe interference correction and would bring the 54Cr/52Cr ratio of np1 to 4.2×solar.”
s-process production in rotating massive stars at solar and low metallicities (2015, background): “The following studies by Limongi, Straniero & Chieffi (2000), Rauscher et al. (2002), The et al. (2007) and Pignatari et al. (2010) confirmed that 22Ne(α, n) is the only important neutron source in C-shell burning, where the remaining 22Ne left after central He-burning is consumed in a very short…”
NanoSIMS: Technical Aspects and Applications in Cosmochemistry and Biological Geochemistry (2013, neutral): “Predictions for different layers in a 15 M SNII (Rauscher et al. 2002) are shown for comparison.”
Nucleosynthesis in the Early Galaxy (2007, background): “The neutron flux duration necessary to obtain a reasonable fit under the lowest neutron density (τ ≈ 1170 years for nn = 10 8 cm−3) far exceeds what is expected by present nucleosynthesis calculations in massive stars (Woosley et al. 2002; Rauscher et al. 2002; Chieffi & Limongi 2004).”
The evolution of the Milky Way from its earliest phases: Constraints on stellar nucleosynthesis (2004, positive): “A recent paper by Rauscher et al. (2002) adopting up to date experimental and theoretical nuclear data, new opacity tables and updated nuclear reaction network and considering stellar evolution with mass loss provided Mg yields higher than the previous ones of WW95 but still not high enough to…”
THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE (2015, background): “…are the main production sites of heavy elements up to the iron group nuclei (e.g., Woosley & Weaver 1995; Hashimoto 1995; Thielemann et al. 1996; Rauscher et al. 2002; Nakamura et al. 2014), have also been expected to provide reliable conditions for the r-process, because the remnant object, a…”
THE COMPACTNESS OF PRESUPERNOVA STELLAR CORES (2013, background): “However, a much larger “adaptive” network of up to 1500 isotopes was carried in parallel with the main structure calculation (Rauscher et al. 2002) and was used to calculate changes in the electron mole number, Ye.”
Non-standard s process in low metallicity massive rotating stars (2011, background): “This site was investigated for the r-process by Truran et al. (1978) and Thielemann et al. (1979), but later on considered only as a possible site for a weak r-process (Woosley et al., 2002) or n-process (Rauscher et al., 2002).”
The s-Process in Massive Stars at Low Metallicity: The Effect of Primary 14N from Fast Rotating Stars (2008, background): “1 Bottom Panel the isotopic distribution without additional 22Ne (case i) is similar to the isotopic distribution at solar metallicity (e.g. Rauscher et al. 2002; Pignatari et al. 2006).”
Nucleosynthesis in multi-dimensional SN Ia explosions (2004, background): “In one spatial dimension it is nowadays possible to solve reaction networks consisting of hundreds of species online with the hydrodynamics (see e.g. Rauscher et al. 2002 for explosive nucleosynthesis calculations in core collapse SNe).”
Evolution, Explosion, and Nucleosynthesis of Core-Collapse Supernovae (2003, neutral): “…Busso & Gallino 1985; Prantzos, Arnould, & Arcoragi 1987; Langer, Arnould, & Arcoragi 1989; Prantzos, Hashimoto, & Nomoto 1990; Raiteri et al. 1991a, 1991b, 1993; Baraffe, El Eid, & Prantzos 1992; The, El Eid, & Meyer 2000; Hoffman, Woosley, & Weaver 2001; Rauscher et al. 2002, hereafter RHHW02).”
SUB-CHANDRASEKHAR MASS MODELS FOR SUPERNOVAE (2010, methodology): “For this study, we used the “adaptive reaction network” described in Rauscher et al. (2002).”
THE REMARKABLE DEATHS OF 9–11 SOLAR MASS STARS (2015, neutral): “The network was “adaptive” (Rauscher et al. 2002).”