268 citations
Counting papers with at most 25 authors, so collaboration author lists do not stand in for the people here.
- K. Sumiyoshi3 profiles91 · h 42
- S. Yamada2 profiles45 · h 47
- S. Furusawa21 · h 20
- H. Nagakura2 profiles19 · h 33
- K. Nakazato18 · h 19
- Akira Harada14 · h 13
- H. Suzuki2 profiles13 · h 14
- Hideyuki Suzuki2 profiles11 · h 8
- W. Iwakami11 · h 19
- Hirotada Okawa10 · h 25
- A. Hosaka2 profiles9 · h 36
- H. Toki2 profiles9 · h 49
- Waseda UniversityJP49 papers
- Kyoto UniversityJP30 papers
- Tokyo University of ScienceJP30 papers
- The University of TokyoJP29 papers
- National Astronomical Observatory of JapanJP21 papers
- RIKENJP19 papers
- High Energy Accelerator Research OrganizationJP16 papers
- The University of OsakaJP14 papers
- Yukawa Institute for Theoretical PhysicsJP12 papers
- Kyushu UniversityJP10 papers
- Princeton UniversityUS9 papers
- Tokyo Institute of TechnologyJP8 papers
111 papers
Bifurcated Impact of Neutrino Fast Flavor Conversion on Core-collapse Supernovae Informed by Multi-angle Neutrino Radiation Hydrodynamics
Ryuichiro Akaho, Hiroki Nagakura, Wakana Iwakami +6
In this {\it Letter}, we present a compelling and robust argument for the roles of neutrino fast flavor conversion (FFC) in the explosion mechanism of core-collapse supernova (CCSN…
Search for nucleon decay via and in 0.484 Mton-year of Super-Kamiokande data
Kamiokande Collaboration, S. Jung, K. Abe +243
We present the results of searches for nucleon decays via and using a 0.484 Mtyr exposure of Super-Kamiokande I-V data covering the…
Long-term neutrino emission from a core-collapse supernova with axion-photon coupling
Masamitsu Mori, Kanji Mori
We perform long-term general-relativistic neutrino-radiation hydrodynamic simulations for core-collapse supernovae (CCSNe) which include the cooling effect induced by the coupling…
Role of symmetry energy at subnuclear densities in protoneutron star crusts
Ken'ichiro Nakazato, Hajime Togashi, Kohsuke Sumiyoshi +1
The impact of matter properties at subnuclear densities on the evolution of protoneutron stars is investigated. Several models of nuclear equation of state (EOS) are constructed wi…
Leptonic and semi-leptonic neutrino interactions with muons in the proto-neutron star cooling
Ken'ichi Sugiura, Shun Furusawa, Kohsuke Sumiyoshi +1
It is known that muons are scarce just after the birth of a proto-neutron star via a supernova explosion but get more abundant as the proto-neutron star cools via neutrino emission…
Effects of nuclear matter and composition in core-collapse supernovae and long-term proto-neutron star cooling
Kohsuke Sumiyoshi, Shun Furusawa, Hiroki Nagakura +4
We study the influence of hot and dense matter in core-collapse supernovae by adopting up-to-date nuclear equation of state (EOS) based on the microscopic nuclear many-body framewo…
Equation of state in neutron stars and supernovae
Kohsuke Sumiyoshi, Toru Kojo, Shun Furusawa
Neutron stars and supernovae provide cosmic laboratories of highly compressed matter at supra nuclear saturation density which is beyond the reach of terrestrial experiments. The p…
Impact of late-time neutrino emission on the diffuse supernova neutrino background
Nick Ekanger, Shunsaku Horiuchi, Kei Kotake +1
In the absence of high-statistics supernova neutrino measurements, estimates of the diffuse supernova neutrino background (DSNB) hinge on the precision of simulations of core-colla…
Protoneutron Star Convection Simulated with a New General Relativistic Boltzmann Neutrino Radiation-Hydrodynamics Code
Ryuichiro Akaho, Akira Harada, Hiroki Nagakura +6
We investigate the protoneutron star (PNS) convection using our newly developed general relativistic Boltzmann neutrino radiation-hydrodynamics code. This is a pilot study for more…
Stability analysis of supermassive primordial stars: a new mass range for general relativistic instability supernovae
Chris Nagele, Hideyuki Umeda, Koh Takahashi +2
Observed supermassive black holes in the early universe have several proposed formation channels, in part because most of these channels are difficult to probe. One of the more pro…
Observing Supernova Neutrino Light Curves with Super-Kamiokande. III. Extraction of Mass and Radius of Neutron Stars from Synthetic Data
Yudai Suwa, Akira Harada, Masayuki Harada +6
Neutrinos are guaranteed to be observable from the next galactic supernova (SN). Optical light and gravitational waves are also observable, but may be difficult to observe if the l…
Equation of state and neutrino transfer in supernovae and neutron stars
Kohsuke Sumiyoshi
We overview the progress of the tables of the equation of state for astrophysical simulations and the numerical methods of neutrino transfer. Hot and dense matter play essential ro…
Principal-Axis Analysis of the Eddington Tensor for the Early Post-Bounce Phase of Rotational Core-Collapse Supernovae
Wakana Iwakami, Akira Harada, Hiroki Nagakura +6
Using full Boltzmann neutrino transport, we performed two-dimensional (2D) core-collapse supernova simulations in axisymmetry for two progenitor models with 11.2M and 15.0M both ro…
Stability of the protoneutron stars toward black hole formation
Hajime Sotani, Kohsuke Sumiyoshi
We examine the protoneutron star (PNS) stability in this study by solving the radial oscillation equations. For this purpose, we adopt the numerical results of massive PNS toward t…
Observing Supernova Neutrino Light Curves with Super-Kamiokande. II. Impact of the Nuclear Equation of State
Ken'ichiro Nakazato, Fumi Nakanishi, Masayuki Harada +6
The late-time evolution of the neutrino event rate from supernovae is evaluated for Super-Kamiokande using simulated results of proto-neutron star (PNS) cooling. In the present wor…
Neutrino emission from the collapse of population III supermassive stars
Chris Nagele, Hideyuki Umeda, Koh Takahashi +2
We calculate the neutrino signal from Population III supermassive star collapse using a neutrino transfer code originally developed for core collapse supernovae and massive star co…
Numerical Study of Stellar Core Collapse and Neutrino Emission Using the Nuclear Equation of State Obtained by the Variational Method
Ken'ichiro Nakazato, Kohsuke Sumiyoshi, Hajime Togashi
Core-collapse simulations of massive stars are performed using the equation of state (EOS) based on the microscopic variational calculation with realistic nuclear forces. The proge…
Developing an end-to-end simulation framework of supernova neutrino detection
Masamitsu Mori, Yudai Suwa, Ken'ichiro Nakazato +5
Massive stars can explode as supernovae at the end of their life cycle, releasing neutrinos whose total energy reaches erg. Moreover, neutrinos play key roles in supernov…
Properties of neutrino transfer in a deformed remnant of neutron star merger
Kohsuke Sumiyoshi, Sho Fujibayashi, Yuichiro Sekiguchi +1
We study properties of neutrino transfer in a remnant of neutron star merger, consisting of a massive neutron star and a surrounding torus. We perform numerical simulations of the…
Multidimensional Boltzmann Neutrino Transport Code in Full General Relativity for Core-collapse Simulations
Ryuichiro Akaho, Akira Harada, Hiroki Nagakura +6
We develop a neutrino transfer code for core-collapse simulations, that directly solves the multidimensional Boltzmann equations in full general relativity. We employ the discrete…
Analytic solutions for neutrino-light curves of core-collapse supernovae
Yudai Suwa, Akira Harada, Ken'ichiro Nakazato +1
Neutrinos are a guaranteed signal from supernova explosions in the Milky Way, and a most valuable messenger that can provide us with information about the deepest parts of supernov…
The Final Fate of Supermassive Pop III Stars: Explosion or Collapse?
Chris Nagele, Hideyuki Umeda, Koh Takahashi +2
We investigate the possibility of a supernova in supermassive () population III stars induced by a general relativistic instability occurring in the helium…
Simulations of the Early Post-Bounce Phase of Core-Collapse Supernovae in Three-Dimensional Space with Full Boltzmann Neutrino Transport
Wakana Iwakami, Hirotada Okawa, Hiroki Nagakura +5
We report on the core-collapse supernova simulation we conducted for a 11.2 M progenitor model in three-dimensional space up to 20 ms after bounce, using a radiation hydrodynamics…
The Boltzmann-radiation-hydrodynamics Simulations of Core-collapse Supernovae with Different Equations of State: the Role of Nuclear Composition and the Behavior of Neutrinos
Akira Harada, Hiroki Nagakura, Wakana Iwakami +5
Using the Boltzmann-radiation-hydrodynamics code, which solves the Boltzmann equation for neutrino transport, we present the results of the simulations with the nuclear equations o…