Implications for Post-processing Nucleosynthesis of Core-collapse Supernova Models with Lagrangian Particles

Harris, J. Austin; Hix, W. R.; Chertkow, Merek A.; Lee, C.-T.; Lentz, Eric J.; Messer, O. E. Bronson

doi:10.3847/1538-4357/aa76de

Cited by 66 publications

(83 citation statements)

References 91 publications

(115 reference statements)

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“…Eichler et al (2017)); and convective blobs from deeper inside can convect neutron-rich layers outwards, leading to weakly neutron-rich conditions (see e.g. Harris et al (2017)). With our PUSH approach, we obtain a similar range of Y e values as found in full multi-dimensional simulations.…”

Section: Summary and Discussionmentioning

confidence: 99%

PUSHing Core-collapse Supernovae to Explosions in Spherical Symmetry. III. Nucleosynthesis Yields

Curtis

Ebinger

Fröhlich

et al. 2018

ApJ

102

104

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In a previously presented proof-of-principle study, we established a parametrized spherically symmetric explosion method (PUSH) that can reproduce many features of core-collapse supernovae for a wide range of pre-explosion models. The method is based on the neutrino-driven mechanism and follows collapse, bounce and explosion. There are two crucial aspects of our model for nucleosynthesis predictions. First, the mass cut and explosion energy emerge simultaneously from the simulation (determining, for each stellar model, the amount of Fe-group ejecta). Second, the interactions between neutrinos and matter are included consistently (setting the electron fraction of the innermost ejecta). In the present paper, we use the successful explosion models from Ebinger et al. (2018) which include two sets of pre-explosion models at solar metallicity, with combined masses between 10.8 and 120 M . We perform systematic nucleosynthesis studies and predict detailed isotopic yields. The resulting 56 Ni ejecta are in overall agreement with observationally derived values from normal core-collapse supernovae. The Fe-group yields are also in agreement with derived abundances for metal-poor star HD 84937. We also present a comparison of our results with observational trends in alpha element to iron ratios.

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Section: Summary and Discussionmentioning

confidence: 99%

PUSHing Core-collapse Supernovae to Explosions in Spherical Symmetry. III. Nucleosynthesis Yields

Curtis

Ebinger

Fröhlich

et al. 2018

ApJ

102

104

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“…WinNet has been used by various authors for r-process nucleosynthesis calculations in core-collapse supernovae and neutron star mergers, and to investigate the impact of nuclear physics on the r-process (e.g., Korobkin et al 2012;Winteler et al 2012;Eichler et al 2015;Martin et al 2015Martin et al , 2016. XNet was developed at Oak Ridge National Laboratories by Hix & Thielemann (1999) and has been used for r-process nucleosynthesis in accretion disk outflows and neutron star mergers, and for explosive nucleosynthesis in type I X-ray bursts and core-collapse supernovae (e.g., Surman et al 2006;Fisker et al 2008;Roberts et al 2011;Harris et al 2017). …”

Section: Network Evolutionmentioning

confidence: 99%

SkyNet: A Modular Nuclear Reaction Network Library

Lippuner

Roberts

2017

ApJS

129

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Almost all of the elements heavier than hydrogen that are present in our solar system were produced by nuclear burning processes either in the early universe or at some point in the life cycle of stars. In all of these environments, there are dozens to thousands of nuclear species that interact with each other to produce successively heavier elements. In this paper, we present SkyNet, a new general-purpose nuclear reaction network that evolves the abundances of nuclear species under the influence of nuclear reactions. SkyNet can be used to compute the nucleosynthesis evolution in all astrophysical scenarios where nucleosynthesis occurs. SkyNet is free and open source, and aims to be easy to use and flexible. Any list of isotopes can be evolved, and SkyNet supports different types of nuclear reactions. SkyNet is modular so that new or existing physics, like nuclear reactions or equations of state, can easily be added or modified. Here, we present in detail the physics implemented in SkyNet with a focus on a self-consistent transition to and from nuclear statistical equilibrium to non-equilibrium nuclear burning, our implementation of electron screening, and coupling of the network to an equation of state. We also present comprehensive code tests and comparisons with existing nuclear reaction networks. We find that SkyNet agrees with published results and other codes to an accuracy of a few percent. Discrepancies, where they exist, can be traced to differences in the physics implementations.

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“…This procedure greatly reduces the number of required trajectories to adequately sample the ejecta: Selecting the final locations of the tracer particles only within the region of interest reduces the total mass of ejecta that must be covered (less than 0.03M ) and makes it easy to use higher mass resolution where it is most needed, i.e., in the neutrino-processed ejecta. For a more general overview of the problems in extracting tracer trajectories from multi-D simulations, we refer the reader to Harris et al (2017).…”

Section: Explosion Dynamicsmentioning

confidence: 99%

Nucleosynthesis in the Innermost Ejecta of Neutrino-driven Supernova Explosions in Two Dimensions

Wanajo

Müller

Janka

et al. 2018

ApJ

176

232

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We examine the nucleosynthesis in the innermost, neutrino-processed ejecta (a few 10 −3 M ) of self-consistent, twodimensional explosion models of core-collapse supernovae for six progenitor stars with different initial masses. Three models have initial masses near the low-mass end of the supernova range, 8.8 M (e8.8; electron-capture supernova), 9.6 M (z9.6), and 8.1 M (u8.1), with initial metallicities of 1, 0, and 10 −4 times the solar metallicity, respectively. The other three are solar-metallicity models with initial masses of 11.2 M (s11), 15 M (s15), and 27 M (s27). The low-mass models e8.8, z9.6, and u8.1 exhibit high production factors (nucleosynthetic abundances relative to the solar ones) of 100-200 for light trans-iron elements from Zn to Zr. This is associated with appreciable ejection of neutron-rich matter in these models. Remarkably, the nucleosynthetic outcomes for progenitors e8.8 and z9.6 are almost identical, including interesting productions of 48 Ca and 60 Fe, irrespective of their quite different (O-Ne-Mg and Fe) cores prior to collapse. In the more massive models s11, s15, and s27, several proton-rich isotopes of light trans-iron elements, including the p-isotope 92 Mo (for s27) are made, up to production factors of ∼30. Both electron-capture and core-collapse supernovae near the low-mass end can therefore be dominant contributors to the Galactic inventory of light trans-iron elements from Zn to Zr and probably 48 Ca and live 60 Fe. The innermost ejecta of more massive supernovae may have only sub-dominant contributions to the chemical enrichment of the Galaxy except for 92 Mo.

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Implications for Post-processing Nucleosynthesis of Core-collapse Supernova Models with Lagrangian Particles

Cited by 66 publications

References 91 publications

PUSHing Core-collapse Supernovae to Explosions in Spherical Symmetry. III. Nucleosynthesis Yields

PUSHing Core-collapse Supernovae to Explosions in Spherical Symmetry. III. Nucleosynthesis Yields

SkyNet: A Modular Nuclear Reaction Network Library

Nucleosynthesis in the Innermost Ejecta of Neutrino-driven Supernova Explosions in Two Dimensions

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