Dynamical Collective Calculation of Supernova Neutrino Signals

Gava, J.; Kneller, James P.; Volpe, Cristina; McLaughlin, G. C.

doi:10.1103/physrevlett.103.071101

Cited by 125 publications

(163 citation statements)

References 42 publications

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“…This selfinduced oscillation process was first discussed in [38] and then explored in a series of papers [39][40][41][42][43][44][45][46]. Thereafter, following the simulations of Duan et al [47,48], it has received much attention recently as a process occurring in the core-collapse supernova environment and leading to flavor conversions of neutrinos and antineutrinos of almost all energies (e.g., [49][50][51][52][53][54][55][56][57][58][59][60][61][62][63][64][65][66][67][68]. Also see the review [69]).…”

Section: Introductionmentioning

confidence: 99%

Role of collective neutrino flavor oscillations in core-collapse supernova shock revival

2012

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We explore the effects of collective neutrino flavor oscillations due to neutrino-neutrino interactions on the neutrino heating behind a stalled core-collapse supernova shock. We carry out axisymmetric (2D) radiation-hydrodynamic core-collapse supernova simulations, tracking the first 400 ms of the post-core-bounce evolution in 11.2-M⊙ and 15-M⊙ progenitor stars. Using inputs from these 2D simulations, we perform neutrino flavor oscillation calculations in multi-energy single-angle and multi-angle single-energy approximations. Our results show that flavor conversions do not set in until close to or outside the stalled shock, enhancing heating by not more than a few percent in the most optimistic case. Consequently, we conclude that the postbounce pre-explosion dynamics of standard core-collapse supernovae remains unaffected by neutrino oscillations. Multi-angle effects in regions of high electron density can further inhibit collective oscillations, strengthening our conclusion.

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Section: Introductionmentioning

confidence: 99%

Role of collective neutrino flavor oscillations in core-collapse supernova shock revival

2012

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“…In between these extreme regimes of synchronized and MSW oscillations, large scale flavor transformation can take place when the neutrino self interaction potential approaches the vacuum oscillation scale [31,32] and the neutrinos and antineutrinos enter the transition region nearly in flavor eigenstates, e.g. [31][32][33][34][35][36][37][38][39]. During the transition, the neutrinos and antineutrinos are said to be "locked" as their survival probabilities mirror each other and the phenomenon is referred to as "bipolar" or "nutation" oscillation.…”

Section: Introductionmentioning

confidence: 99%

Symmetric and standard matter neutrino resonances above merging compact objects

2016

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Matter-neutrino resonances (MNR) can occur in environments where the flux of electron antineutrinos is greater than the flux of electron neutrinos. These resonances may result in dramatic neutrino flavor transformation. Compact object merger disks are an example of an environment where electron antineutrinos outnumber neutrinos. We study MNR resonances in several such disk configurations and find two qualitatively different types of matter-neutrino resonances: a standard MNR and a symmetric MNR. We examine the transformation that occurs in each type of resonance and explore the consequences for nucleosynthesis.

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“…For the most part the various neutrino flavor transformation processes have been studied in isolation, see Gava et al [65] for an exception, but of course the neutrino signal is the denouement involving all these protagonists. In order to understand the explosion narrative we must determine which process left which features in the signal and how they interacted.…”

Section: Introductionmentioning

confidence: 99%

“…The flavor transformation due to the MSW effect is also non-trivial because the passage of the shock wave through the star leaves an impression in the signal [50,[60][61][62][63][64][65]. A further complication is the possible presence of density fluctuations/turbulence [30,[66][67][68][69][70][71] which one would expect to be created by the large scale inhomogeneities generated during the accretion phase.…”

Section: Introductionmentioning

confidence: 99%

Combining collective, MSW, and turbulence effects in supernova neutrino flavor evolution

Lund¹,

Kneller²

2013

Phys. Rev. D

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In order to decode the neutrino burst signal from a Galactic core-collapse supernova (ccSN) and reveal the complicated inner workings of the explosion we need a thorough understanding of the neutrino flavor evolution from the proto-neutron star outwards. The flavor content of the signal evolves due to both neutrino collective effects and matter effects which can lead to a highly interesting interplay and distinctive spectral features. In this paper we investigate the supernova neutrino flavor evolution in three different progenitors and include collective flavor effects, the evolution of the Mikheyev, Smirnov & Wolfenstein (MSW) conversion due to the shock wave passage through the star, and the impact of turbulence. We consider both normal and inverted neutrino mass hierarchies and a value of θ13 close to the current experimental measurements. In the Oxygen-Neon-Magnesium (ONeMg) supernova we find that the impact of turbulence is both brief and slight during a window of 1-2 seconds post bounce. This is because the shock races through the star extremely quickly and the turbulence amplitude is expected to be small, less than 10%, since these stars do not require multi-dimensional physics to explode. Thus the spectral features of collective and shock effects in the neutrino signals from Oxygen-Neon-Magnesium supernovae may be almost turbulence free making them the easiest to interpret. For the more massive progenitors we again find that small amplitude turbulence, up to 10%, leads to a minimal modification of the signal, and the emerging neutrino spectra retain both collective and MSW features. However, when larger amounts of turbulence is added, 30% and 50%, which is justified by the requirement of multi-dimensional physics in order to make these stars explode, the features of collective and shock wave effects in the high (H) density resonance channel are almost completely obscured at late times. Yet at the same time we find the other mixing channels -the low (L) density resonance channel and the non-resonant channels -begin to develop turbulence signatures. Large amplitude turbulent motions in the outer layers of more massive, iron core-collapse supernovae may obscure the most obvious fingerprints of collective and shock wave effects in the neutrino signal but cannot remove them completely, and additionally bring about new features in the signal.

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Dynamical Collective Calculation of Supernova Neutrino Signals

Cited by 125 publications

References 42 publications

Role of collective neutrino flavor oscillations in core-collapse supernova shock revival

Role of collective neutrino flavor oscillations in core-collapse supernova shock revival

Symmetric and standard matter neutrino resonances above merging compact objects

Combining collective, MSW, and turbulence effects in supernova neutrino flavor evolution

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