Supernova Neutrinos: Production, Oscillations and Detection

By A. Mirizzi, I. Tamborra, Hans-Thomas Janka, N. Saviano, Kate Scholberg, R. Bollig, Lorenz Hudepohl, S. Chakraborty. 2015

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Neutrinos play a crucial role in the collapse and explosion of massive stars, governing the infall dynamics of the stellar core, triggering and fueling the explosion and driving the cooling and deleptonization of the newly formed neutron star. Due to their role neutrinos carry information from the heart of the explosion and, due to their weakly interacting nature, offer the only direct probe of the dynamics and thermodynamics at the center of a supernova. In this paper, we review the present status of modelling the neutrino physics and signal formation in collapsing and exploding stars. We assess the capability of current and planned large underground neutrino detectors to yield faithful information of the time and flavor dependent neutrino signal from a future Galactic supernova. We show how the observable neutrino burst would provide a benchmark for fundamental supernova physics with unprecedented richness of detail. Exploiting the treasure of the measured neutrino events requires a careful discrimination of source-generated properties from signal features that originate on the way to the detector. As for the latter, we discuss self-induced flavor conversions associated with neutrino-neutrino interactions that occur in the deepest stellar regions; matter effects that modify the pattern of flavor conversions in the dynamical stellar envelope; neutrino-oscillation signatures that result from structural features associated with the shock-wave propagation as well as turbulent mass motions in post-shock layers. Finally, we highlight our current understanding of the formation of the diffuse supernova neutrino background and we analyse the perspectives for a detection of this relic signal that integrates the contributions from all past core-collapse supernovae in the Universe.

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Citations in the corpus

Volume I. Introduction to DUNE (2020, background): “The information in a supernova neutrino burst (SNB) available in principle to be gathered by experimentalists is the flavor, energy and time structure of a several-tens-of-second-long, all-flavor, few-tens-of-MeV neutrino burst [19, 20].”
What can be learned from a future supernova neutrino detection (2017, methodology): “For each, we first show in parenthesis the number of events in the dominant channel for the largest detector in its class, taken from Table I of [11], where a canonical distance to the core collapse of 10 kpc is used.”
CORE-COLLAPSE SUPERNOVAE FROM 9 TO 120 SOLAR MASSES BASED ON NEUTRINO-POWERED EXPLOSIONS (2015, methodology): “This is shown in Figure 6, where we plot the time evolution of the 1.1 M cores for two self-consistent PNS cooling simulations with all relevant microphysics (Mirizzi et al. 2015), carried out with the nuclear EOS of Lattimer & Swesty (1991).”
Self-induced neutrino flavor conversion without flavor mixing (2016, background): “ents [1{3]. However, a true understanding of avor evolution in dense environments has remained elusive because of many complications engendered by the nonlinear nature of collective avor oscillations [3,4]. We study a new item on this list which has eluded most workers in this eld with the notable e”
Origin of the heaviest elements: The rapid neutron-capture process (2019, background): “neutron star (Roberts et al., 2012; Mirizzi et al., 2016) have shown that most or all of the ejecta are protonrich.”
DARWIN: towards the ultimate dark matter detector (2016, background): “Neutrinos and anti-neutrinos of all flavours are emitted by core-collapse supernovae in a burst lasting a few tens of seconds [86].”
Deep Underground Neutrino Experiment (DUNE), Far Detector Technical Design Report, Volume II: DUNE Physics (2020, background): “The information in a supernova neutrino burst available in principle to be gathered by experimentalists is the flavor, energy and time structure of several-tens-of-second-long, all-flavor, fewtens-of-MeV neutrino burst [42, 43].”
Muonic Boson Limits: Supernova Redux (2021, unknown): “After the explosion, probably some hundreds of ms after collapse, the evolution of the remaining proto neutron star (PNS) is deleptonization and cooling on a diffusion time scale of a few seconds because neutrinos are trapped [54–56].”