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YAMADA S, NAGAKURA H, AKAHO R, HARADA A, FURUSAWA S, IWAKAMI W, OKAWA H, MATSUFURU H, SUMIYOSHI K. Physical mechanism of core-collapse supernovae that neutrinos drive. PROCEEDINGS OF THE JAPAN ACADEMY. SERIES B, PHYSICAL AND BIOLOGICAL SCIENCES 2024; 100:190-233. [PMID: 38462501 PMCID: PMC11105976 DOI: 10.2183/pjab.100.015] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/05/2023] [Accepted: 12/05/2023] [Indexed: 03/12/2024]
Abstract
The current understanding of the mechanism of core-collapse supernovae (CCSNe), one of the most energetic events in the universe associated with the death of massive stars and the main formation channel of compact objects such as neutron stars and black holes, is reviewed for broad readers from different disciplines of science who may not be familiar with the object. Therefore, we emphasize the physical aspects than the results of individual model simulations, although large-scale high-fidelity simulations have played the most important roles in the progress we have witnessed in the past few decades. It is now believed that neutrinos are the most important agent in producing the commonest type of CCSNe. The so-called neutrino-heating mechanism will be the focus of this review and its crucial ingredients in micro- and macrophysics and in numerics will be explained one by one. We will also try to elucidate the remaining issues.
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Affiliation(s)
- Shoichi YAMADA
- Department of Physics, Faculty of Science and Engineering, Waseda University, Tokyo, Japan
- Research Institute for Science and Engineering, Waseda University, Tokyo, Japan
| | - Hiroki NAGAKURA
- National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
| | - Ryuichiro AKAHO
- Department of Physics, Faculty of Science and Engineering, Waseda University, Tokyo, Japan
| | - Akira HARADA
- Interdisciplinary Theoretical and Mathematical Sciences Program (iTHEMS), RIKEN, Wako, Saitama, Japan
| | - Shun FURUSAWA
- College of Science and Engineering, Kanto Gakuin University, Yokohama, Kanagawa, Japan
| | - Wakana IWAKAMI
- Department of Physics, Faculty of Science and Engineering, Waseda University, Tokyo, Japan
| | - Hirotada OKAWA
- Waseda Institute for Advanced Study, Waseda University, Tokyo, Japan
| | - Hideo MATSUFURU
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki, Japan
| | - Kohsuke SUMIYOSHI
- National Institute of Technology, Numazu College, Numazu, Shizuoka, Japan
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Abstract
The coalescence of double neutron star (NS-NS) and black hole (BH)-NS binaries are prime sources of gravitational waves (GW) for Advanced LIGO/Virgo and future ground-based detectors. Neutron-rich matter released from such events undergoes rapid neutron capture (r-process) nucleosynthesis as it decompresses into space, enriching our universe with rare heavy elements like gold and platinum. Radioactive decay of these unstable nuclei powers a rapidly evolving, approximately isotropic thermal transient known as a "kilonova", which probes the physical conditions during the merger and its aftermath. Here I review the history and physics of kilonovae, leading to the current paradigm of day-timescale emission at optical wavelengths from lanthanide-free components of the ejecta, followed by week-long emission with a spectral peak in the near-infrared (NIR). These theoretical predictions, as compiled in the original version of this review, were largely confirmed by the transient optical/NIR counterpart discovered to the first NS-NS merger, GW170817, discovered by LIGO/Virgo. Using a simple light curve model to illustrate the essential physical processes and their application to GW170817, I then introduce important variations about the standard picture which may be observable in future mergers. These include ∼ hour-long UV precursor emission, powered by the decay of free neutrons in the outermost ejecta layers or shock-heating of the ejecta by a delayed ultra-relativistic outflow; and enhancement of the luminosity from a long-lived central engine, such as an accreting BH or millisecond magnetar. Joint GW and kilonova observations of GW170817 and future events provide a new avenue to constrain the astrophysical origin of the r-process elements and the equation of state of dense nuclear matter.
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Affiliation(s)
- Brian D. Metzger
- Department of Physics, Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027 USA
- Center for Computational Astrophysics, Flatiron Institute, New York, NY 10010 USA
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Bollig R, Janka HT, Lohs A, Martínez-Pinedo G, Horowitz CJ, Melson T. Muon Creation in Supernova Matter Facilitates Neutrino-Driven Explosions. PHYSICAL REVIEW LETTERS 2017; 119:242702. [PMID: 29286734 DOI: 10.1103/physrevlett.119.242702] [Citation(s) in RCA: 14] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/14/2017] [Indexed: 06/07/2023]
Abstract
Muons can be created in nascent neutron stars (NSs) due to the high electron chemical potentials and the high temperatures. Because of their relatively lower abundance compared to electrons, their role has so far been ignored in numerical simulations of stellar core collapse and NS formation. However, the appearance of muons softens the NS equation of state, triggers faster NS contraction, and thus leads to higher luminosities and mean energies of the emitted neutrinos. This strengthens the postshock heating by neutrinos and can facilitate explosions by the neutrino-driven mechanism.
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Affiliation(s)
- R Bollig
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, 85748 Garching, Germany
- Physik Department, Technische Universität München, James-Franck-Straße 1, 85748 Garching, Germany
| | - H-T Janka
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, 85748 Garching, Germany
| | - A Lohs
- GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany
| | - G Martínez-Pinedo
- GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany
- Institut für Kernphysik (Theoriezentrum), Technische Universität Darmstadt, Schlossgartenstraße 2, 64289 Darmstadt, Germany
| | - C J Horowitz
- Nuclear Theory Center and Department of Physics, Indiana University, Bloomington, Indiana 47408, USA
| | - T Melson
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, 85748 Garching, Germany
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Abstract
The mergers of double neutron star (NS-NS) and black hole (BH)-NS binaries are promising gravitational wave (GW) sources for Advanced LIGO and future GW detectors. The neutron-rich ejecta from such merger events undergoes rapid neutron capture (r-process) nucleosynthesis, enriching our Galaxy with rare heavy elements like gold and platinum. The radioactive decay of these unstable nuclei also powers a rapidly evolving, supernova-like transient known as a "kilonova" (also known as "macronova"). Kilonovae are an approximately isotropic electromagnetic counterpart to the GW signal, which also provides a unique and direct probe of an important, if not dominant, r-process site. I review the history and physics of kilonovae, leading to the current paradigm of week-long emission with a spectral peak at near-infrared wavelengths. Using a simple light curve model to illustrate the basic physics, I introduce potentially important variations on this canonical picture, including: [Formula: see text]day-long optical ("blue") emission from lanthanide-free components of the ejecta; [Formula: see text]hour-long precursor UV/blue emission, powered by the decay of free neutrons in the outermost ejecta layers; and enhanced emission due to energy input from a long-lived central engine, such as an accreting BH or millisecond magnetar. I assess the prospects of kilonova detection following future GW detections of NS-NS/BH-NS mergers in light of the recent follow-up campaign of the LIGO binary BH-BH mergers.
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Affiliation(s)
- Brian D. Metzger
- Columbia Astrophysics Laboratory, Department of Physics, Columbia University, New York, NY USA
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Spyrou A, Liddick SN, Naqvi F, Crider BP, Dombos AC, Bleuel DL, Brown BA, Couture A, Crespo Campo L, Guttormsen M, Larsen AC, Lewis R, Möller P, Mosby S, Mumpower MR, Perdikakis G, Prokop CJ, Renstrøm T, Siem S, Quinn SJ, Valenta S. Strong Neutron-γ Competition above the Neutron Threshold in the Decay of ^{70}Co. PHYSICAL REVIEW LETTERS 2016; 117:142701. [PMID: 27740831 DOI: 10.1103/physrevlett.117.142701] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/18/2016] [Indexed: 06/06/2023]
Abstract
The β-decay intensity of ^{70}Co was measured for the first time using the technique of total absorption spectroscopy. The large β-decay Q value [12.3(3) MeV] offers a rare opportunity to study β-decay properties in a broad energy range. Two surprising features were observed in the experimental results, namely, the large fragmentation of the β intensity at high energies, as well as the strong competition between γ rays and neutrons, up to more than 2 MeV above the neutron-separation energy. The data are compared to two theoretical calculations: the shell model and the quasiparticle random phase approximation (QRPA). Both models seem to be missing a significant strength at high excitation energies. Possible interpretations of this discrepancy are discussed. The shell model is used for a detailed nuclear structure interpretation and helps to explain the observed γ-neutron competition. The comparison to the QRPA calculations is done as a means to test a model that provides global β-decay properties for astrophysical calculations. Our work demonstrates the importance of performing detailed comparisons to experimental results, beyond the simple half-life comparisons. A realistic and robust description of the β-decay intensity is crucial for our understanding of nuclear structure as well as of r-process nucleosynthesis.
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Affiliation(s)
- A Spyrou
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
| | - S N Liddick
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Chemistry, Michigan State University, East Lansing, Michigan 48824, USA
| | - F Naqvi
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
| | - B P Crider
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
| | - A C Dombos
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
| | - D L Bleuel
- Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, California 94550-9234, USA
| | - B A Brown
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
| | - A Couture
- Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
| | - L Crespo Campo
- Department of Physics, University of Oslo, NO-0316 Oslo, Norway
| | - M Guttormsen
- Department of Physics, University of Oslo, NO-0316 Oslo, Norway
| | - A C Larsen
- Department of Physics, University of Oslo, NO-0316 Oslo, Norway
| | - R Lewis
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Chemistry, Michigan State University, East Lansing, Michigan 48824, USA
| | - P Möller
- Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
| | - S Mosby
- Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
| | - M R Mumpower
- Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
| | - G Perdikakis
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
- Central Michigan University, Mt. Pleasant, Michigan 48859, USA
| | - C J Prokop
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Chemistry, Michigan State University, East Lansing, Michigan 48824, USA
| | - T Renstrøm
- Department of Physics, University of Oslo, NO-0316 Oslo, Norway
| | - S Siem
- Department of Physics, University of Oslo, NO-0316 Oslo, Norway
| | - S J Quinn
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
| | - S Valenta
- Faculty of Mathematics and Physics, Charles University in Prague, V Holešovičkách 2, CZ-180 00 Prague 8, Czech Republic
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