Grand unified neutrino spectrum at Earth: Sources and spectral components

Vitagliano, Edoardo; Tamborra, Irene; Raffelt, Georg G.

doi:10.1103/revmodphys.92.045006

Cited by 108 publications

(93 citation statements)

References 471 publications

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“…, and E = 10 4 MeV, Figure 2b shows the temporal evolution of the angle-integrated off-diagonal term of the density matrix based on the predictions of the linear stability analysis and the numerical solution of the equations of motion (Equations 1 and 2). 1 The linear stability analysis perfectly agrees with the numerical solution in the linear regime, but it cannot give any insight into the nonlinear evolution of the density matrix. The linear stability analysis aims to predict whether the (anti)neutrino ensemble may develop flavor instabilities for given initial conditions.…”

Section: Linear Stability Analysismentioning

confidence: 78%

“…Core-collapse supernovae represent the final life stage for stars with masses of at least 8 M ࣻ (1,(12)(13)(14)(15). A supernova is effectively a blackbody source of (anti)neutrinos of all flavors; when the stellar core collapses, neutrinos carry 99% of the gravitational binding energy (E b ∼ 3 × 10 53 erg).…”

Section: Core-collapse Supernovaementioning

confidence: 99%

“…Neutrinos are among the most abundant particles in our Universe and play a pivotal role in a variety of astrophysical environments that range from the sun to the most energetic transients (1). Neutrinos interact weakly and have the unique property of changing their flavor while propagating.…”

Section: Introductionmentioning

confidence: 99%

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New Developments in Flavor Evolution of a Dense Neutrino Gas

Tamborra

Shalgar

2021

Annu. Rev. Nucl. Part. Sci.

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152

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Neutrino–neutrino refraction dominates the flavor evolution in core-collapse supernovae, neutron star mergers, and the early Universe. Ordinary neutrino flavor conversions develop on timescales determined by the vacuum oscillation frequency. However, when the neutrino density is large enough, collective flavor conversions may arise because of pairwise neutrino scattering. Pairwise conversions are deemed fast because they are expected to occur on timescales that depend on the neutrino–neutrino interaction energy (i.e., on the neutrino number density) and are regulated by the angular distributions of electron neutrinos and antineutrinos. The enigmatic phenomenon of fast pairwise conversions has been overlooked for a long time. However, because of the fast conversion rate, pairwise conversions could occur in the proximity of the neutrino decoupling region with yet-to-be-understood implications for the hydrodynamics of astrophysical sources and the synthesis of the heavy elements. We review the physics of this fascinating phenomenon and its implications for neutrino-dense sources. Expected final online publication date for the Annual Review of Nuclear and Particle Science, Volume 71 is September 2021. Please see http://www.annualreviews.org/page/journal/pubdates for revised estimates.

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Section: Linear Stability Analysismentioning

confidence: 78%

Section: Core-collapse Supernovaementioning

confidence: 99%

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New Developments in Flavor Evolution of a Dense Neutrino Gas

Tamborra

Shalgar

2021

Annu. Rev. Nucl. Part. Sci.

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152

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“…Neutrinos are produced from a variety of sources across a wide energy range as shown in Fig. 3.1 [7]. They can come from cosmic rays scattering with CMB photons, astrophysical sources, atmospheric cosmic ray showers, nuclear reactors, the Sun, and the Earth [7].…”

Section: Neutrino Sourcesmentioning

confidence: 99%

“…3.1 [7]. They can come from cosmic rays scattering with CMB photons, astrophysical sources, atmospheric cosmic ray showers, nuclear reactors, the Sun, and the Earth [7]. At the lowest end of the energy spectrum, the neutrinos that come from the cosmic neutrino background (CνB) and from big bang nucleosynthesis (BBN) have yet to be detected due to the high energy resolution that would be required to detect them.…”

Section: Neutrino Sourcesmentioning

confidence: 99%

Dark matter neutrino scattering in the galactic centre with IceCube

McMullen¹,

Vincent²,

Argüelles³

et al. 2021

J. Inst.

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While there is evidence for the existence of dark matter, its properties have yet to be discovered. Simultaneously, the nature of high-energy astrophysical neutrinos detected by IceCube remains unresolved. If dark matter and neutrinos are coupled to each other, they could exhibit a non-zero elastic scattering cross section. Such an interaction between an isotropic extragalactic neutrino flux and dark matter would be concentrated in the Galactic Centre, where the dark matter column density is the greatest. This scattering would attenuate the flux of high-energy neutrinos, which could be observed in the IceCube South Pole Neutrino Observatory. In this thesis, an unbinned likelihood analysis is performed to set sensitivities for the seven year medium energy starting event cascades dataset for a signal considering possible dark matterneutrino interaction scenarios. This signal would be observed as a suppression of the high-energy astrophysical neutrino flux in the direction of the Galactic Centre. It is shown that IceCube can set constraints on possible dark matter-neutrino interactions that are complementary to constraints set by large scale structure surveys and the cosmic microwave background. i I would like to thank my supervisor Aaron Vincent at Queen's and co-supervisor Carlos Argüelles at Harvard for their support and guidance during the course of this thesis. I have been extremely lucky to have great supervisors who patiently answer all my questions and provide invaluable advice. I would also like to thank Austin Schneider for his excellent insight with this analysis. I would like to acknowledge the support of NSERC, the IceCube collaboration, the Frontenac Cluster, and the Canadian Armed Forces in making this thesis possible. I would also like to thank all my family and friends for their support during this degree. I would especially like to thank Eric and Mikayla McMullen for editing this thesis and Simran Nerval for providing feedback for my thesis presentation. I would also like to thank the members of my thesis committee, Joe Bramante and Nahee Park for their comments and discussion during the thesis defence.

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Diffuse Supernova Neutrino Background

Suliga

2022

Handbook of Nuclear Physics

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Grand unified neutrino spectrum at Earth: Sources and spectral components

Cited by 108 publications

References 471 publications

New Developments in Flavor Evolution of a Dense Neutrino Gas

New Developments in Flavor Evolution of a Dense Neutrino Gas

Dark matter neutrino scattering in the galactic centre with IceCube

Diffuse Supernova Neutrino Background

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