Neutrino bounds on astrophysical sources and new physics

Anchordoqui, Luis A.; Feng, Jonathan L.; Goldberg, Haim; Shapere, Alfred D.

doi:10.1103/physrevd.66.103002

Cited by 180 publications

(338 citation statements)

References 112 publications

(72 reference statements)

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“…The region with the solid boundary is obtained by a cosmological evolution parameter n = 3. Boxes show the upper bounds obtained by combining Fly's Eye [13] and Agasa [14] limits on deeply penetrating showers in different energy bins [15]. According to these limits, strong cosmological evolution (n > 3) for the sources of the post-GZK events is already excluded.…”

Section: Propagation Inversionmentioning

confidence: 99%

“…The variation due to the change of this parameter between 0 and 6 is also shown. Present [15] and expected [16] experimental bounds by AGASA, Fly's Eye and Auger, respectively, are also presented.…”

Section: Propagation Inversionmentioning

confidence: 99%

“…(4)). Boxes show the upper bounds obtained by combining Fly's Eye [13] and Agasa [14] limits on deeply-penetrating showers in different energy bins [15]. The dotted band labelled by Auger represents the expected sensitivity of the Pierre Auger Observatory to ν τ +ν τ , corresponding to one event per year per energy decade [16].…”

Section: Propagation Functionsmentioning

confidence: 99%

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Bounds on the cosmogenic neutrino flux

Fodor¹,

Katz²,

Ringwald³

et al. 2003

J. Cosmol. Astropart. Phys.

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Under the assumption that some part of the observed highest energy cosmic rays consists of protons originating from cosmological distances, we derive bounds on the associated flux of neutrinos generated by inelastic processes with the cosmic microwave background photons. We exploit two methods. First, a power-like injection spectrum is assumed. Then, a modelindependent technique, based on the inversion of the observed proton flux, is presented. The inferred lower bound is quite robust. As expected, the upper bound depends on the unknown composition of the highest energy cosmic rays. Our results represent benchmarks for all ultrahigh energy neutrino telescopes.

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Section: Propagation Inversionmentioning

confidence: 99%

Section: Propagation Inversionmentioning

confidence: 99%

Section: Propagation Functionsmentioning

confidence: 99%

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Bounds on the cosmogenic neutrino flux

Fodor¹,

Katz²,

Ringwald³

et al. 2003

J. Cosmol. Astropart. Phys.

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“…A eff , T live and ε are all energy dependent. Methods set out in [77,92,105] show that equation 8.1.1 underestimates the limit that can be placed on the UHE neutrino flux. Equation 8.1.1 effectively places an upper limit on the flux at any given neutrino energy for the number of events observed, while the desired limit should account for neutrino flux models providing neutrinos over the energy interval being considered.…”

Section: Diffuse Uhe Neutrino Flux Limitmentioning

confidence: 99%

A Search for Ultra-High Energy Neutrinos and Cosmic-Rays with ANITA-2

Mottram¹

2012

Springer Theses

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“…One could thus claim with confidence that black holes with masses 5 to 20 times the Planck scale, depending on the model of quantum gravity, could form in the collision of particles at the CERN LHC is the Planck scale was low enough. Early phenomenological studies can be found in [8][9][10][11][12][13][14]. …”

mentioning

confidence: 99%

Quantum Black Holes and Effective Quantum Gravity Approaches

Calmet

2015

Springer Proceedings in Physics

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One of the most exciting developments in theoretical physics in the last 20 years has been the realization that the scale of quantum gravity could be in the TeV region instead of the usually assumed 10 19 GeV. Indeed, the strength of gravity can be affected by the size of potential extra-dimensions [1][2][3][4] or the quantum fluctuations of a large hidden sector of particles [5]. A dramatic signal of quantum gravity in the TeV region would be the production of small black holes in high energy collisions of particles at colliders. The possibility of creating small black holes at colliders has led to some wonderful theoretical works on the formation of black holes in the collisions of particles.Long before studying the production of such black holes in the high energy collisions of particles became fashionable, in the 1970's Penrose proved that a closed trapped surface forms when two shockwaves traveling at energies much larger than the Planck scale even when the impact parameter is non-zero. Unfortunately, he never published his work. The result was independently rediscovered by Eardley and Giddings in 2002 [6] when the high energy community started to discuss the formation of black holes at colliders. Earlier estimate of the production cross section had been done using the hoop conjecture. Some did not trust the hoop conjecture, thinking that in the collision of particles the situation was too asymmetrical to trust this conjecture. The paper of Eardley and Giddings settled the issue. Proving the formation of a closed trapped surface is enough to establish gravitational collapse and hence the formation of a black hole. This work was extended by Hsu [7] into the semi-classical region using path integral methods. One could thus claim with confidence that black holes with masses 5 to 20 times the Planck scale, depending on the model of quantum gravity, could form in the collision of particles at the CERN LHC is the Planck scale was low enough. Early phenomenological studies can be found in [8][9][10][11][12][13][14].

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Neutrino bounds on astrophysical sources and new physics

Cited by 180 publications

References 112 publications

Bounds on the cosmogenic neutrino flux

Bounds on the cosmogenic neutrino flux

A Search for Ultra-High Energy Neutrinos and Cosmic-Rays with ANITA-2

Quantum Black Holes and Effective Quantum Gravity Approaches

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