Echo Technique to Distinguish Flavors of Astrophysical Neutrinos

Li, Shirley Weishi; Bustamante, Mauricio; Beacom, J. F.

doi:10.1103/physrevlett.122.151101

Cited by 37 publications

(42 citation statements)

References 78 publications

(85 reference statements)

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“…The behavior with energy scales monotonically, as shown in the right-hand panel of Fig. 8, noting that the second and third peak are perfectly correlated (as also shown in [43]). We therefore use π + as a proxy for hadrons, and electrons for electromagnetic showers.…”

Section: Cherenkov Timing and Light Echossupporting

confidence: 59%

“…Ref. [43] found that this leads to a distinctive three-peak signature in the time-evolution of the Cherenkov light produced by a high-energy neutrino. The first peak, which crests around 10 −7 s is the largest, and comes from the immediate energy deposition by primary particles.…”

Section: Cherenkov Timing and Light Echosmentioning

confidence: 99%

“…We note one improvement with respect to the analysis in Ref. [43]: rather than treating hadronic events as a single hadron, we will include the full effects of hadronization with the aid of Pythia, which leads to slightly more overlap between NC and CC events.…”

Section: Cherenkov Timing and Light Echosmentioning

confidence: 99%

“…It was shown in Ref. [43] that the initial Cherenkov shower produced by neutrino-nucleus deep inelastic scattering (DIS) events is followed by a delayed muon decay signal around 10 −6 s after the initial interaction, and thereafter by a third peak due to neutron capture at 10 −3 s. The size of the neutron peak relative to the total energy can be used as a proxy for the shower composition. We will show that in the peak ratio/energy deposition plane, evaporating BHs occupy a specific region, which may allow them to be differentiated from standard charged current and neutral current interactions on a statistical basis.…”

mentioning

confidence: 99%

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Signatures of microscopic black holes and extra dimensions at future neutrino telescopes

Mack

Song

Vincent

2020

J. High Energ. Phys.

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In scenarios with large extra dimensions (LEDs), the fundamental Planck scale can be low enough that collisions between high-energy particles may produce microscopic black holes. High-energy cosmic neutrinos can carry energies much larger than a PeV, opening the door to a higher energy range than Earth-based colliders. Here, for the first time, we identify a number of unique signatures of microscopic black holes as they would appear in the next generation of large-scale neutrino observatories such as IceCube-Gen2 and the Pacific Ocean Neutrino Explorer. These signatures include new event topologies, energy distributions, and unusual ratios of hadronic-to-electronic energy deposition, visible through Cherenkov light echos due to delayed neutron recombination. We find that the next generation of neutrino telescopes can probe LEDs with a Planck scale up to 6 TeV, though the identification of unique topologies could push their reach even further. I. INTRODUCTIONAmong the diverse signatures of new physics above the TeV scale, the possibility of producing microscopic black holes in particle collisions remains one of the most alluring. In models with Large Extra Dimensions (LEDs), the large hierarchy between gravity and the electroweak scales can be at least partly explained by confining the Standard Model (SM) gauge interactions to a 3+1-dimensional brane, while allowing gravity to "leak" into one or more extra bulk dimensions [1][2][3][4][5][6]. This allows a true Planck scale M that can be much lower than the observed M P l ∼ 10 18 GeV. Such scenarios have been tested extensively in terms of gravitational force tests [7], supernova and neutron star cooling [8,9], and in collider experiments [10,11]. If only one LED exists, Solar System-scale modifications of Newtonian gravity [1] prohibit a TeV-scale Planck mass. However, two or more LEDs remain allowed by observation. Current constraints limit the scale M to be above about 3 -25 TeV [7][8][9][10][11][12], depending on the number of extra dimensions.A vastly-reduced Planck scale also allows for the creation of microscopic black holes (BHs) in the collision between two high-energy particles with centre of mass (CM) energy E CM M , a smoking gun signature of extra dimensions. The hoop conjecture [13] tells us that a black hole will form if the impact parameter b between two colliding particles is smaller than twice the horizon radius r H of a black hole with mass M • = E CM . This has mainly been studied in the context of high-energy colliders [14][15][16][17][18][19][20][21][22][23][24][25][26] by searching for the high-multiplicity signature from rapid Hawking evaporation [27]. The reach of collider experiments is limited by the finite CM collision energy. Cosmic accelerators thus provide an alluring alternative, as high-energy cosmic rays can reach much higher momenta. This has been known for some time, and extensive studies have been performed on the production of BHs in air showers [28][29][30][31][32][33][34][35], particularly if they are observed with energies a...

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Section: Cherenkov Timing and Light Echossupporting

confidence: 59%

Section: Cherenkov Timing and Light Echosmentioning

confidence: 99%

Section: Cherenkov Timing and Light Echosmentioning

confidence: 99%

mentioning

confidence: 99%

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Signatures of microscopic black holes and extra dimensions at future neutrino telescopes

Mack

Song

Vincent

2020

J. High Energ. Phys.

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“…We briefly summarize the neutrino detection techniques used in IceCube and similar detectors [2,3,88,89]. Neutrinos interact with nuclei and electrons, producing relativistic particles that emit Cherenkov light that is detected by photomultiplier tubes.…”

Section: B Review Of Detection In Icecubementioning

confidence: 99%

W -boson and trident production in TeV–PeV neutrino observatories

Zhou

Beacom

2020

Phys. Rev. D

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Detecting TeV-PeV cosmic neutrinos provides crucial tests of neutrino physics and astrophysics. The statistics of IceCube and the larger proposed IceCube-Gen2 demand calculations of neutrinonucleus interactions subdominant to deep-inelastic scattering, which is mediated by weak-boson couplings to nuclei. The largest such interactions are W -boson and trident production, which are mediated instead through photon couplings to nuclei. In a companion paper [1], we make the most comprehensive and precise calculations of those interactions at high energies. In this paper, we study their phenomenological consequences. We find that: (1) These interactions are dominated by the production of on-shell W -bosons, which carry most of the neutrino energy, (2) The cross section on water/iron can be as large as 7.5%/14% that of charged-current deep-inelastic scattering, much larger than the quoted uncertainty on the latter, (3) Attenuation in Earth is increased by as much as 15%, (4) W -boson production on nuclei exceeds that through the Glashow resonance on electrons by a factor of 20 for the best-fit IceCube spectrum, (5) The primary signals are showers that will significantly affect the detection rate in IceCube-Gen2; a small fraction of events give unique signatures that may be detected sooner.

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The ultra-high-energy neutrino-nucleon cross section: measurement forecasts for an era of cosmic EeV-neutrino discovery

Valera

Bustamante

Gläser

2022

J. High Energ. Phys.

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Neutrino interactions with protons and neutrons probe their deep structure and may reveal new physics. The higher the neutrino energy, the sharper the probe. So far, the neutrino-nucleon (νN) cross section is known across neutrino energies from a few hundred MeV to a few PeV. Soon, ultra-high-energy (UHE) cosmic neutrinos, with energies above 100 PeV, could take us farther. So far, they have evaded discovery, but upcoming UHE neutrino telescopes endeavor to find them. We present the first detailed measurement forecasts of the UHE νN cross section, geared to IceCube-Gen2, one of the leading detectors under planning. We use state-of-the-art ingredients in every stage of our forecasts: in the UHE neutrino flux predictions, the neutrino propagation inside Earth, the emission of neutrino-induced radio signals in the detector, their propagation and detection, and the treatment of backgrounds. After 10 years, if at least a few tens of UHE neutrino-induced events are detected, IceCube-Gen2 could measure the νN cross section at center-of-mass energies of $$ \sqrt{s} $$ s ≈ 10–100 TeV for the first time, with a precision comparable to that of its theory prediction.

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Echo Technique to Distinguish Flavors of Astrophysical Neutrinos

Cited by 37 publications

References 78 publications

Signatures of microscopic black holes and extra dimensions at future neutrino telescopes

Signatures of microscopic black holes and extra dimensions at future neutrino telescopes

W -boson and trident production in TeV–PeV neutrino observatories

The ultra-high-energy neutrino-nucleon cross section: measurement forecasts for an era of cosmic EeV-neutrino discovery

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