Cosmic absorption of ultra high energy particles

Ruffini, Remo; Vereshchagin, Gregory; Xue, She‐Sheng

doi:10.1007/s10509-016-2668-5

Cited by 25 publications

(20 citation statements)

References 57 publications

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“…The horizon imposed by the Bethe-Heitler process is instead defined by the mean energy-loss distance, corresponding to the distance at which the energy of the UHECR has fallen to 1/e of its original value. For the Bethe-Heitler process this distance is 1 Gpc (Ruffini et al 2016), which sets the effective horizon for UHECR protons with energies less than E GZK .…”

Section: Other Propagation Effectsmentioning

confidence: 99%

An Upper Limit on the Strength of the Extragalactic Magnetic Field from Ultra-high-energy Cosmic-Ray Anisotropy

Bray

Scaife

2018

ApJ

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If ultra-high-energy cosmic rays originate from extragalactic sources, the offsets of their arrival directions from these sources imply an upper limit on the strength of the extragalactic magnetic field (EGMF). The Pierre Auger Collaboration has recently reported that anisotropy in the arrival directions of cosmic rays is correlated with several types of extragalactic objects. If these cosmic rays originate from these objects, they imply a limit on the EGMF strength of B<0.7-2.2 10 1 MpcMpc and B< 0.7-2.2×10−10 G at larger scales. This is comparable to existing upper limits at λ B =1 Mpc, and improves on them by a factor of 4-12 at larger scales. The principal source of uncertainty in our results is the unknown cosmicray composition.

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Section: Other Propagation Effectsmentioning

confidence: 99%

An Upper Limit on the Strength of the Extragalactic Magnetic Field from Ultra-high-energy Cosmic-Ray Anisotropy

Bray

Scaife

2018

ApJ

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“…A guaranteed example for EeV neutrinos is the GZK or cosmogenic neutrinos produced by the scattering of the cosmic ray off photons of the CMB. Considering that the CMB is distributed uniformly all over the universe without clustering in any halo, the mean free path of protons with energy exceeding 5×10 19 eV is 6 Mpc [34] which is larger than the halo size. That is even if the cosmic ray originates in a halo with large ρ DM , the production of the neutrinos will take place outside the halo where ρ DM is smaller than ∼ 10 −5 times ρ DM in the halo.…”

Section: Jhep07(2021)174mentioning

confidence: 99%

On the τ flavor of the cosmic neutrino flux

Farzan

2021

J. High Energ. Phys.

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Observation of high energy cosmic neutrinos by ICECUBE has ushered in a new era in exploring both cosmos and new physics beyond the Standard Model (SM). In the standard picture, although mostly νμ and νe are produced in the source, oscillation will produce ντen route. Certain beyond SM scenarios, like interaction with ultralight DM can alter this picture. Thus, the flavor composition of the cosmic neutrino flux can open up the possibility of exploring certain beyond the SM scenarios that are inaccessible otherwise. We show that the τ flavor holds a special place among the neutrino flavors in elucidating new physics. Interpreting the two anomalous events observed by ANITA as ντ events makes the tau flavor even more intriguing. We study how the detection of the two tau events by ICECUBE constrains the interaction of the neutrinos with ultralight dark matter and discuss the implications of this interaction for even higher energy cosmic neutrinos detectable by future radio telescopes such as ARA, ARIANNA and GRAND. We also revisit the 3 + 1 neutrino scheme as a solution to the two anomalous ANITA events and clarify a misconception that exists in the literature about the evolution of high energy neutrinos in matter within the 3 + 1 scheme with a possibility of scattering off nuclei. We show that the existing bounds on the flux of ντ with energy of EeV rules out this solution for the ANITA events. We show that the 3 + 1 solution can be saved from both this bound and from the bound on the extra relativistic degrees of freedom in the early universe by turning on the interaction of neutrinos with ultralight dark matter.

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“…A guaranteed example for EeV neutrinos is the GZK or cosmogenic neutrinos produced by the scattering of the cosmic ray off photons of the CMB. Considering that the CMB is distributed uniformly all over the universe without clustering in any halo, the mean free path of protons with energy exceeding 5 × 10 19 eV is 6 Mpc [26] which is larger than the halo size. That is even if the cosmic ray originates in a halo with large ρ DM , the production of the neutrinos will take place outside the halo where ρ DM is smaller than ∼ 10 −5 times ρ DM in the halo.…”

Section: Interaction With Ultralight Dark Mattermentioning

confidence: 99%

On the Tau flavor of the cosmic neutrino flux

Farzan

2021

Preprint

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Observation of high energy cosmic neutrinos by ICECUBE has ushered in a new era in exploring both cosmos and new physics beyond the Standard Model (SM). In the standard picture, although mostly ν µ and ν e are produced in the source, oscillation will produce ν τ en route. Certain beyond SM scenarios, like interaction with ultralight DM can alter this picture. Thus, the flavor composition of the cosmic neutrino flux can open up the possibility of exploring certain beyond the SM scenarios that are inaccessible otherwise. We show that the τ flavor holds a special place among the neutrino flavors in elucidating new physics.Interpreting the two anomalous events observed by ANITA as ν τ events makes the tau flavor even more intriguing. We study how the detection of the two tau events by ICECUBE constrains the interaction of the neutrinos with ultralight dark matter and discuss the implications of this interaction for even higher energy cosmic neutrinos detectable by future radio telescopes such as ARA, ARIANNA and GRAND. We also revisit the 3 + 1 neutrino scheme as a solution to the two anomalous ANITA events and clarify a misconception that exists in the literature about the evolution of high energy neutrinos in matter within the 3 + 1 scheme with a possibility of scattering off nuclei. We show that the existing bounds on the flux of ν τ with energy of EeV rules out this solution for the ANITA events. We show that the 3 + 1 solution can be saved from both this bound and from the bound on the extra relativistic degrees of freedom in the early universe by turning on the interaction of neutrinos with ultralight dark matter.

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Cosmic absorption of ultra high energy particles

Cited by 25 publications

References 57 publications

An Upper Limit on the Strength of the Extragalactic Magnetic Field from Ultra-high-energy Cosmic-Ray Anisotropy

An Upper Limit on the Strength of the Extragalactic Magnetic Field from Ultra-high-energy Cosmic-Ray Anisotropy

On the τ flavor of the cosmic neutrino flux

On the Tau flavor of the cosmic neutrino flux

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