The KM3NeT potential for the next core-collapse supernova observation with neutrinos

AbstractThe KM3NeT research infrastructure is under construction in the Mediterranean Sea. It consists of two water Cherenkov neutrino detectors, ARCA and ORCA, aimed at neutrino astrophysics and oscillation research, respectively. Instrumenting a large volume of sea water with $$\sim {6200}$$ ∼ 6200 optical modules comprising a total of $$\sim {200{,}000}$$ ∼ 200 , 000 photomultiplier tubes, KM3NeT will achieve sensitivity to $$\sim {10} \ \mathrm{MeV}$$ ∼ 10 MeV neutrinos from Galactic and near-Galactic core-collapse supernovae through the observation of coincident hits in photomultipliers above the background. In this paper, the sensitivity of KM3NeT to a supernova explosion is estimated from detailed analyses of background data from the first KM3NeT detection units and simulations of the neutrino signal. The KM3NeT observational horizon (for a $$5\,\sigma $$ 5 σ discovery) covers essentially the Milky-Way and for the most optimistic model, extends to the Small Magellanic Cloud ($$\sim {60} \ \mathrm{kpc}$$ ∼ 60 kpc ). Detailed studies of the time profile of the neutrino signal allow assessment of the KM3NeT capability to determine the arrival time of the neutrino burst with a few milliseconds precision for sources up to 5–8 kpc away, and detecting the peculiar signature of the standing accretion shock instability if the core-collapse supernova explosion happens closer than 3–5 kpc, depending on the progenitor mass. KM3NeT’s capability to measure the neutrino flux spectral parameters is also presented.

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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.

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Global Anisotropy versus Small‐Scale Fluctuations in Neutrino Flux in Core‐Collapse Supernova Explosions

The Astrophysical Journal ◽

10.1086/375833 ◽

2003 ◽

Vol 592 (2) ◽

pp. 1035-1041 ◽

Cited By ~ 5

Author(s):

Hideki Madokoro ◽

Tetsuya Shimizu ◽

Yuko Motizuki

Keyword(s):

Neutrino Flux ◽

Small Scale ◽

Core Collapse ◽

Core Collapse Supernova ◽

Supernova Explosions

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Time Profile of the Neutrino Burst from the Supernova 1987A

International Astronomical Union Colloquium ◽

10.1017/s0252921100094252 ◽

1988 ◽

Vol 108 ◽

pp. 426-427

Author(s):

Hideyuki Suzuki ◽

Katsuhiko Sato

Keyword(s):

Monte Carlo ◽

Neutrino Flux ◽

Supernova Explosion ◽

Time Profile ◽

The Other ◽

Late Time ◽

The Core ◽

Supernova 1987A ◽

Theoretical Predictions ◽

First Time

SN1987A gave us the first opportunity to study the supernova core directly by providing us the neutrino signal from the core. The observational data of the neutrino flux detected by Kamiokande[1] and IMB[2] show surprisingly good agreements with the theoretical predictions as a whole[3,4]. The fundamental concept of the collapse driven supernova explosion is confirmed for the first time. On the other hand, there are some puzzles. The most peculiar feature of the data is the 7 seconds gap of the Kamiokande data. The first 8 events of Kamiokande were detected in 2 seconds, following the 7 seconds gap and the last 3 events in 4 seconds. Of course just only 7 seconds gap is not unnatural if small neutrino flux come. But there were detected 3 events after the gap. These 3 events may not be produced by the weak flux. We can estimate the time integrated luminosity of corresponding to the last 3 events and get the large value such as 7 · 1052erg [5]. Can we get out of this inconsistency, 3 events after the 7 seconds gap? If not, we may need to consider some nonstandard mechanism of the neutrino emission at the late time. In order to investigate the probability of the case in which there is a 7 seconds gap before 3 events, we have performed Monte Carlo simulations for the simple model of neutrino flux.

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A successful 3D core-collapse supernova explosion model

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/sty2585 ◽

2018 ◽

Vol 482 (1) ◽

pp. 351-369 ◽

Cited By ~ 64

Author(s):

David Vartanyan ◽

Adam Burrows ◽

David Radice ◽

M Aaron Skinner ◽

Joshua Dolence

Keyword(s):

Supernova Explosion ◽

Core Collapse ◽

Core Collapse Supernova

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Effects of Small-Scale Fluctuations of Neutrino Flux in Supernova Explosions

International Astronomical Union Colloquium ◽

10.1017/s0252921100009349 ◽

2005 ◽

Vol 192 ◽

pp. 309-314

Author(s):

Hideki Madokoro ◽

Tetsuya Shimizu ◽

Yuko Motizuki

Keyword(s):

Neutrino Flux ◽

Explosion Energy ◽

Small Scale ◽

Core Collapse ◽

Effective Mechanism ◽

Core Collapse Supernova ◽

Neutrino Radiation ◽

Spherical Explosion ◽

Supernova Explosions ◽

Neutrino Luminosity

SummaryWe examine effects of small-scale fluctuations with angle in the neutrino radiation in core-collapse supernova explosions. As the mode number of fluctuations increases, the results approach those of spherical explosion. We conclude that global anisotropy of the neutrino radiation is the most effective mechanism of increasing the explosion energy when the total neutrino luminosity is given.

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Acoustic wave generation in collapsing massive stars with convective shells

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa533 ◽

2020 ◽

Vol 493 (3) ◽

pp. 3496-3512 ◽

Cited By ~ 1

Author(s):

Ernazar Abdikamalov ◽

Thierry Foglizzo

Keyword(s):

Acoustic Waves ◽

Massive Stars ◽

Core Collapse ◽

Core Collapse Supernova ◽

Stellar Collapse ◽

Acoustic Wave Generation ◽

Supernova Explosions ◽

Accretion Shock ◽

Stationary Background ◽

Hydrodynamics Equations

ABSTRACT The convection that takes place in the innermost shells of massive stars plays an important role in the formation of core-collapse supernova explosions. Upon encountering the supernova shock, additional turbulence is generated, amplifying the explosion. In this work, we study how the convective perturbations evolve during the stellar collapse. Our main aim is to establish their physical properties right before they reach the supernova shock. To this end, we solve the linearized hydrodynamics equations perturbed on a stationary background flow. The latter is approximated by the spherical transonic Bondi accretion, while the convective perturbations are modelled as a combination of entropy and vorticity waves. We follow their evolution from large radii, where convective shells are initially located, down to small radii, where they are expected to encounter the accretion shock above the proto-neutron star. Considering typical vorticity perturbations with a Mach number ∼0.1 and entropy perturbations with magnitude ∼0.05kb/baryon, we find that the advection of these perturbations down to the shock generates acoustic waves with a relative amplitude $\delta {\rm p}/\gamma {\rm p} \lesssim 10{{\ \rm per\ cent}}$, in agreement with published numerical simulations. The velocity perturbations consist of contributions from acoustic and vorticity waves with values reaching ${\sim}10{{\ \rm per\ cent}}$ of the sound speed ahead of the shock. The perturbation amplitudes decrease with increasing ℓ and initial radii of the convective shells.

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