Dynamics and Equation of State Dependencies of Relevance for Nucleosynthesis in Supernovae and Neutron Star Mergers

Hans-Thomas Janka⁴ &
Andreas Bauswein⁵

87 Accesses
3 Citations

Abstract

Neutron stars (NSs) and black holes (BHs) are born when the final collapse of the stellar core terminates the lives of stars more massive than about nine solar masses. This can trigger the powerful ejection of a large fraction of the star’s material in a core-collapse supernova (CCSN), whose extreme luminosity is energized mostly by the decay of radioactive isotopes such as ⁵⁶Ni and its daughter nucleus ⁵⁶Co. When evolving in close binary systems, the compact relics of such infernal catastrophes spiral towards each other on orbits gradually decaying by gravitational wave emission. Ultimately, the violent collision of the two components forms a more massive, rapidly spinning remnant, again accompanied by the ejection of considerable amounts of matter. These merger events can be observed by high-energy bursts of gamma rays with afterglows and electromagnetic transients called kilonovae, which radiate the energy released in radioactive decays of freshly assembled rapid neutron-capture elements. By means of their mass ejection and the nuclear and neutrino reactions taking place in the ejecta, both CCSNe and compact object mergers (COMs) are prominent sites of heavy-element nucleosynthesis and play a central role in the cosmic cycle of matter and the chemical enrichment history of galaxies. The nuclear equation of state (EoS) of NS matter, from neutron-rich to proton-dominated conditions and with temperatures ranging from about 0 to roughly 100 MeV, is a crucial ingredient in these astrophysical phenomena. It determines their dynamical processes, their remnant properties even at the level of deciding between NS or BH, and the properties of the associated emission of neutrinos, whose interactions govern the thermodynamic conditions and the neutron-to-proton ratio for nucleosynthesis reactions in the innermost ejecta. This chapter discusses corresponding EoS-dependent effects of relevance in CCSNe as well as COMs.

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Dynamics and Equation of State Dependencies of Relevance for Nucleosynthesis in Supernovae and Neutron Star Mergers

r-Process Nucleosynthesis from Compact Binary Mergers

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Acknowledgements

HTJ is grateful for support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) through Sonderforschungsbereich (Collaborative Research Center) SFB 1258 “Neutrinos and Dark Matter in Astro- and Particle Physics (NDM)” and under Germany’s Excellence Strategy through Cluster of Excellence ORIGINS (EXC-2094)-390783311. AB acknowledges support by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program under grant agreement No. 759253, support by DFG – Project-ID 279384907 – SFB 1245 and DFG – Project-ID 138713538 – SFB 881 (“The Milky Way System”, subproject A10) and support by the State of Hesse within the Cluster Project ELEMENTS.

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Hans-Thomas Janka
GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt, Germany
Andreas Bauswein

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Research Center for Nuclear Physics, Osaka University, Ibaraki, Osaka, Japan
Isao Tanihata
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Hiroshi Toki
National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
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Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1, DE 85748, Garching, Germany
Hans-Thomas Janka

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Janka, HT., Bauswein, A. (2023). Dynamics and Equation of State Dependencies of Relevance for Nucleosynthesis in Supernovae and Neutron Star Mergers. In: Tanihata, I., Toki, H., Kajino, T. (eds) Handbook of Nuclear Physics . Springer, Singapore. https://doi.org/10.1007/978-981-15-8818-1_93-1

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Dynamics and Equation of State Dependencies of Relevance for Nucleosynthesis in Supernovae and Neutron Star Mergers

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Dynamics and Equation of State Dependencies of Relevance for Nucleosynthesis in Supernovae and Neutron Star Mergers

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Dynamics and Equation of State Dependencies of Relevance for Nucleosynthesis in Supernovae and Neutron Star Mergers

r-Process Nucleosynthesis from Compact Binary Mergers

r-Process Nucleosynthesis from Compact Binary Mergers

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