scholarly journals Neutrino Emission as Diagnostics of Core-Collapse Supernovae

2019 ◽  
Vol 69 (1) ◽  
pp. 253-278 ◽  
Author(s):  
B. Müller
Keyword(s):  
Particle Physics ◽  
Core Collapse ◽  
Open Problems ◽  
Neutrino Detectors ◽  
Core Collapse Supernova ◽  
Cooling Phase ◽  
Neutrino Fluxes ◽  
Bulk Parameters ◽  
Shed Light ◽  
Proto Neutron Star

With myriads of detection events from a prospective Galactic core-collapse supernova, current and future neutrino detectors will be able to sample detailed, time-dependent neutrino fluxes and spectra. This will offer significant possibilities of inferring supernova physics from the various phases of the neutrino signal, ranging from the neutronization burst through the accretion and early explosion phases to the cooling phase. The signal will constrain the time evolution of bulk parameters of the young proto–neutron star, such as its mass and radius, as well as the structure of the progenitor; probe multidimensional phenomena in the supernova core; and constrain the dynamics of the early explosion phase. Aside from further astrophysical implications, supernova neutrinos may also shed light on the properties of matter at supranuclear densities and on open problems in particle physics.

scholarly journals Probing neutrino decay scenarios by using the Earth matter effects on supernova neutrinos

2022 ◽  
Vol 2022 (01) ◽  
pp. 003
Author(s):  
Edwin A. Delgado ◽  
Hiroshi Nunokawa ◽  
Alexander A. Quiroga
Keyword(s):  
Core Collapse ◽  
Neutrino Detectors ◽  
Core Collapse Supernova ◽  
Matter Effects ◽  
The Earth ◽  
Two Factors ◽  
Matter Effect ◽  
The Difference ◽  
Neutrino Fluxes ◽  
Neutrino Decay

Abstract The observation of Earth matter effects in the spectrum of neutrinos coming from a next galactic core-collapse supernova (CCSN) could, in principle, reveal if neutrino mass ordering is normal or inverted. One of the possible ways to identify the mass ordering is through the observation of the modulations that appear in the spectrum when neutrinos travel through the Earth before they arrive at the detector. These features in the neutrino spectrum depend on two factors, the average neutrino energies, and the difference between the primary neutrino fluxes of electron and other flavors produced inside the supernova. However, recent studies indicate that the Earth matter effect for CCSN neutrinos is expected to be rather small and difficult to be observed by currently operating or planned neutrino detectors mainly because of the similarity of average energies and fluxes between electron and other flavors of neutrinos, unless the distance to CCSN is significantly smaller than the typically expected one, ∼ 10 kpc. Here, we are looking towards the possibility if the non-standard neutrino properties such as decay of neutrinos can enhance the Earth matter effect. In this work we show that invisible neutrino decay can potentially enhance significantly the Earth matter effect for both νe and ν̅e channels at the same time for both mass orderings, even if the neutrino spectra between electron and other flavors of neutrinos are very similar, which is a different feature not expected for CCSN neutrinos with standard oscillation without the decay effect.

scholarly journals A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations

2020 ◽  
Vol 492 (4) ◽  
pp. 5764-5779 ◽  
Author(s):  
Hiroki Nagakura ◽  
Adam Burrows ◽  
David Radice ◽  
David Vartanyan
Keyword(s):  
Neutron Star ◽  
Systematic Study ◽  
Three Dimensional ◽  
Three Dimensions ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
Tau Neutrinos ◽  
The Impact ◽  
Proto Neutron Star

ABSTRACT This paper presents the first systematic study of proto-neutron star (PNS) convection in three dimensions (3D) based on our latest numerical fornax models of core-collapse supernova (CCSN). We confirm that PNS convection commonly occurs, and then quantify the basic physical characteristics of the convection. By virtue of the large number of long-term models, the diversity of PNS convective behaviour emerges. We find that the vigour of PNS convection is not correlated with CCSN dynamics at large radii, but rather with the mass of PNS − heavier masses are associated with stronger PNS convection. We find that PNS convection boosts the luminosities of νμ, ντ, $\bar{\nu }_{\mu }$, and $\bar{\nu }_{\tau }$ neutrinos, while the impact on other species is complex due to a competition of factors. Finally, we assess the consequent impact on CCSN dynamics and the potential for PNS convection to generate pulsar magnetic fields.

Recent Status of Multi-Dimensional Core-Collapse Supernova Models

2015 ◽  
Vol 11 (A29A) ◽  
pp. 340-344
Author(s):  
Kei Kotake ◽  
Ko Nakamura ◽  
Tomoya Takiwaki
Keyword(s):  
Energy Transport ◽  
Unique Feature ◽  
Three Dimensional ◽  
Radiation Hydrodynamics ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
Self Consistent ◽  
New Type ◽  
Explosion Mechanism ◽  
Proto Neutron Star

AbstractWe report a recent status of multi-dimensional neutrino-radiation hydrodynamics simulations for clarifying the explosion mechanism of core-collapse supernovae (CCSNe). In this contribution, we present two results, one from two-dimensional (2D) simulations using multiple progenitor models and another from three-dimensional (3D) rotational core-collapse simulation using a single progenitor. From the first ever systematic 2D simulations, it is shown that the compactness parameter ξ that characterizes the structure of the progenitors is a key to diagnose the explodability of neutrino-driven explosions. In the 3D rotating model, we find a new type of rotation-assisted explosion, which makes the explosion energy bigger than that in the non-rotating model. The unique feature has not been captured in previous 2D self-consistent rotational models because the growth of non-axisymmetric instabilities is the key to foster the explosion by enhancing the energy transport from the proto-neutron star to the gain region.

scholarly journals Offline performance studies and first real-timeresults on Core-Collapse Supernova neutrinosearches with the KM3NeT neutrino detectors

2019 ◽  
Author(s):  
Marta Colomer Molla ◽  
Alexis Coleiro ◽  
Damien Dornic ◽  
Vladimir Kulikovskiy ◽  
Massimiliano Lincetto ◽  
...  
Keyword(s):  
Performance Studies ◽  
Core Collapse ◽  
Neutrino Detectors ◽  
Core Collapse Supernova

scholarly journals Neutrino fluxes from a core-collapse supernova in a model with three sterile neutrinos

2016 ◽  
Vol 42 (12) ◽  
pp. 800-814 ◽  
Author(s):  
A. V. Yudin ◽  
D. K. Nadyozhin ◽  
V. V. Khruschov ◽  
S. V. Fomichev
Keyword(s):  
Core Collapse ◽  
Sterile Neutrinos ◽  
Core Collapse Supernova ◽  
Neutrino Fluxes

scholarly journals Temporal and angular variations of 3D core-collapse supernova emissions and their physical correlations

2019 ◽  
Vol 489 (2) ◽  
pp. 2227-2246 ◽  
Author(s):  
David Vartanyan ◽  
Adam Burrows ◽  
David Radice
Keyword(s):  
Neutron Star ◽  
Gravitational Wave ◽  
3D Models ◽  
Temporal Variations ◽  
Neutrino Energy ◽  
Mode Frequency ◽  
Core Collapse ◽  
Time Dynamics ◽  
Core Collapse Supernova ◽  
Proto Neutron Star

Abstract We provide the time series and angular distributions of the neutrino and gravitational wave emissions of 11 state-of-the-art 3D non-rotating core-collapse supernova models and explore correlations between these signatures and the real-time dynamics of the shock and the proto-neutron star (PNS) core. The neutrino emissions are roughly isotropic on average, with instantaneous excursions about the mean inferred luminosity of as much as ±20 per cent. The deviation from isotropy is least for the ‘νμ’-type neutrinos and the lowest mass progenitors. Instantaneous temporal luminosity variations along a given direction for exploding models average ∼2–4 per cent, but can be as high as ∼10 per cent. For non-exploding models, they can achieve ∼25 per cent. The temporal variations in the neutrino emissions correlate with the temporal and angular variations in the mass accretion rate. We witness the lepton-number emission self-sustained asymmetry (LESA) phenomenon in all our models and find that the vector direction of the LESA dipole and that of the inner Ye distribution are highly correlated. For our entire set of 3D models, we find strong connections between the cumulative neutrino energy losses, the radius of the proto-neutron star, and the f-mode frequency of the gravitational wave emissions. When physically normalized, the progenitor-to-progenitor variation in any of these quantities is no more than ∼10 per cent. Moreover, the reduced f-mode frequency is independent of time after bounce to better than ∼10 per cent. Therefore, simultaneous measurement of gravitational waves and neutrinos from a given supernova event can be used synergistically to extract real physical quantities of the supernova core.

Non-exploding and exploding core-collapse supernova models and the multimessenger predictions

2019 ◽  
Vol 15 (S350) ◽  
pp. 267-273
Author(s):  
Kei Kotake ◽  
Takami Kuroda ◽  
Tomoya Takiwaki
Keyword(s):  
Black Hole ◽  
Massive Star ◽  
Three Dimensional ◽  
Core Collapse ◽  
Rapid Rotation ◽  
Core Collapse Supernova ◽  
Collapse Simulation ◽  
Collapse Model ◽  
General Relativistic ◽  
Proto Neutron Star

AbstractWe present results of full general relativistic (GR), three-dimensional (3D) core-collapse simulation of a massive star with multi-energy neutrino transport. Using a 70Mȯ zero-metallicity star, we show that the black-hole (BH) formation occurs at ∼ 300 ms after bounce. At a few ∼ 10 ms before the BH formation, we find that the stalled bounce shock is revived by neutrino heating from the forming hot proto-neutron star (PNS), which is aided by vigorous convection behind the shock. Our numerical results present the first evidence to validate the BH formation by the so-called fallback scenario. Furthermore we present results from a rapidly rotating core-collapse model of a 27Mȯ star that is trending towards an explosion. We point out that the correlated neutrino and gravitational-wave signatures, if detected, could provide a smoking-gun evidence of rapid rotation of the newly-born PNS.

scholarly journals Wave heating from proto-neutron star convection and the core-collapse supernova explosion mechanism

2019 ◽  
Vol 491 (4) ◽  
pp. 5376-5391 ◽  
Author(s):  
Sarah E Gossan ◽  
Jim Fuller ◽  
Luke F Roberts
Keyword(s):  
Acoustic Waves ◽  
Supernova Explosion ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
The Core ◽  
Shock Region ◽  
Wave Heating ◽  
Post Shock ◽  
Explosion Mechanism ◽  
Proto Neutron Star

ABSTRACT Our understanding of the core-collapse supernova explosion mechanism is incomplete. While the favoured scenario is delayed revival of the stalled shock by neutrino heating, it is difficult to reliably compute explosion outcomes and energies, which depend sensitively on the complex radiation hydrodynamics of the post-shock region. The dynamics of the (non-)explosion depend sensitively on how energy is transported from inside and near the proto-neutron star (PNS) to material just behind the supernova shock. Although most of the PNS energy is lost in the form of neutrinos, hydrodynamic and hydromagnetic waves can also carry energy from the PNS to the shock. We show that gravity waves excited by core PNS convection can couple with outgoing acoustic waves that present an appreciable source of energy and pressure in the post-shock region. Using one-dimensional simulations, we estimate the gravity wave energy flux excited by PNS convection and the fraction of this energy transmitted upwards to the post-shock region as acoustic waves. We find wave energy fluxes near $10^{51}\, \mathrm{erg}\, \mathrm{s}^{-1}\,$ are likely to persist for $\sim \! 1\, \mathrm{s}$ post-bounce. The wave pressure on the shock may exceed $10{{\ \rm per\ cent}}$ of the thermal pressure, potentially contributing to shock revival and, subsequently, a successful and energetic explosion. We also discuss how future simulations can better capture the effects of waves, and more accurately quantify wave heating rates.

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

2019 ◽  
Vol 209 ◽  
pp. 01009 ◽  
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.

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