Exploring the Potential of Multi-Detector Analyses for Core-Collapse Supernova Neutrino Detection

Core Collapse Supernovae (CCSNe) are explosive phenomena that may occur at the end of the life of massive stars, releasing over 99% of the energy through neutrino emission. While the explosion mechanism is not fully understood, neutrinos are believed to play an important role. The only detection as of today are the 24 neutrinos from SN1987A. The observation of the next Galactic CCSN will lead to important breakthroughs in astroparticle physics. For a Galactic CCSN, the KM3NeT ORCA and ARCA detectors in the Mediterranean Sea will observe a significant neutrino signal via the detection of Cherenkov light, mostly induced by Inverse Beta Decay interactions in sea water. The detection of coincident photons by the 31 photomultipliers of each KM3NeT digital optical module (DOM) allows for an efficient discrimination of the optical backgrounds. The KM3NeT detection sensitivity to a Galactic CCSN and the potential to resolve the neutrino light-curve have been estimated relying on detailed Monte Carlo simulations. Specific criteria are proposed for the online triggering and the participation in the SNEWS network.

Download Full-text

Core-Collapse Supernova neutrino detection prospects with the KM3NeT neutrino telescopes.

EPJ Web of Conferences ◽

10.1051/epjconf/201920901009 ◽

2019 ◽

Vol 209 ◽

pp. 01009 ◽

Cited By ~ 1

Author(s):

Marta Colomer Molla ◽

Massimiliano Lincetto

Keyword(s):

Particle Physics ◽

Sea Water ◽

Detection Sensitivity ◽

Core Collapse ◽

Neutrino Telescopes ◽

Core Collapse Supernova ◽

Inverse Beta Decay ◽

Optical Background ◽

Supernova Neutrino ◽

Explosion Mechanism

Core Collapse Supernovae (CCSN) are explosive phenomena that may occur at the end of the life of massive stars, releasing over 99% of the energy through neutrino emission with energies on the 10 MeV scale. While the explosion mechanism is not fully understood, neutrinos are believed to play an important role. The only detection as of today are the 24 neutrinos from supernova SN1987A. The observation of the next Galactic CCSN will lead to important breakthroughs across the fields of astrophysics, nuclear and particle physics. For a Galactic CCSN, the KM3NeT ORCA and ARCA detectors in the Mediterranean Sea will observe a significant number of neutrinos via the detection of Cherenkov light, mostly induced by Inverse Beta Decay (IBD) interactions in sea water. The detection of coincident photons by the 31 photomultipliers of the KM3NeT digital optical modules (DOMs) allows to separate the signal from the optical background sources. The KM3NeT detection sensitivity to a Galactic CCSN and the potential to resolve the neutrino light-curve have been estimated exploiting detailed Monte-Carlo simulations. Specific criteria are proposed for the online triggering and the participation in the SNEWS network.

Download Full-text

Analytical approximation of neutrino distribution function in core-collapse supernova

Journal of Physics Conference Series ◽

10.1088/1742-6596/1690/1/012003 ◽

2020 ◽

Vol 1690 ◽

pp. 012003

Author(s):

A Dobrynina ◽

E Koptyaeva ◽

I Ognev

Keyword(s):

Distribution Function ◽

Analytical Approximation ◽

Core Collapse ◽

Core Collapse Supernova

Download Full-text

Deep learning for core-collapse supernova detection

Physical Review D ◽

10.1103/physrevd.103.063011 ◽

2021 ◽

Vol 103 (6) ◽

Author(s):

M. López ◽

I. Di Palma ◽

M. Drago ◽

P. Cerdá-Durán ◽

F. Ricci

Keyword(s):

Deep Learning ◽

Core Collapse ◽

Core Collapse Supernova

Download Full-text

High-z core-collapse supernova survey with shock breakout

10.1063/1.4754357 ◽

2012 ◽

Author(s):

Nozomu Tominaga ◽

Tomoki Morokuma ◽

Sergei I. Blinnikov

Keyword(s):

Core Collapse ◽

Core Collapse Supernova

Download Full-text

Core Collapse Supernova Models and Nucleosynthesis

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313009198 ◽

2013 ◽

Vol 9 (S296) ◽

pp. 27-36

Author(s):

Ken'ichi Nomoto

Keyword(s):

Big Bang ◽

Elemental Abundance ◽

Core Collapse ◽

Solar Abundance ◽

First Stars ◽

Abundance Pattern ◽

Core Collapse Supernova ◽

Abundance Patterns ◽

Supernova Explosions ◽

The Big Bang

AbstractAfter the Big Bang, production of heavy elements in the early Universe takes place in the first stars and their supernova explosions. The nature of the first supernovae, however, has not been well understood. The signature of nucleosynthesis yields of the first supernovae can be seen in the elemental abundance patterns observed in extremely metal-poor stars. Interestingly, those abundance patterns show some peculiarities relative to the solar abundance pattern, which should provide important clues to understanding the nature of early generations of supernovae. We review the recent results of the nucleosynthesis yields of massive stars. We examine how those yields are affected by some hydrodynamical effects during the supernova explosions, namely, explosion energies from those of hypernovae to faint supernovae, mixing and fallback of processed materials, asphericity, etc. Those parameters in the supernova nucleosynthesis models are constrained from observational data of supernovae and metal-poor stars.

Download Full-text

Importance of 56Ni production on diagnosing explosion mechanism of core-collapse supernova

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/sty3309 ◽

2018 ◽

Vol 483 (3) ◽

pp. 3607-3617 ◽

Cited By ~ 9

Author(s):

Yudai Suwa ◽

Nozomu Tominaga ◽

Keiichi Maeda

Keyword(s):

Core Collapse ◽

Core Collapse Supernova ◽

Explosion Mechanism

Download Full-text

A shallow water analogue of asymmetric core-collapse, and neutron star kick/spin

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312012811 ◽

2011 ◽

Vol 7 (S279) ◽

pp. 134-137

Author(s):

Thierry Foglizzo ◽

Frédéric Masset ◽

Jérôme Guilet ◽

Gilles Durand

Keyword(s):

Neutron Star ◽

Shallow Water ◽

Acoustic Waves ◽

Large Scale ◽

Massive Stars ◽

Core Collapse ◽

Hydraulic Jumps ◽

Core Collapse Supernova ◽

Accretion Shock

AbstractMassive stars end their life with the gravitational collapse of their core and the formation of a neutron star. Their explosion as a supernova depends on the revival of a spherical accretion shock, located in the inner 200km and stalled during a few hundred milliseconds. Numerical simulations suggest that the large scale asymmetry of the neutrino-driven explosion is induced by a hydrodynamical instability named SASI. Its non radial character is able to influence the kick and the spin of the resulting neutron star. The SWASI experiment is a simple shallow water analog of SASI, where the role of acoustic waves and shocks is played by surface waves and hydraulic jumps. Distances in the experiment are scaled down by a factor one million, and time is slower by a factor one hundred. This experiment is designed to illustrate the asymmetric nature of core-collapse supernova.

Download Full-text