UHE neutrino damping in a thermal gas of relic neutrinos

D’Olivo, Juan Carlos; Nellen, L.; Sahu, Sarira; Elewyck, V. Van

doi:10.1016/j.astropartphys.2005.11.005

Cited by 12 publications

(24 citation statements)

References 32 publications

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“…where bar denotes antiparticle, f is a fermion. It has a typical Breit-Wigner shape and is given in the analytic form in [23]. We take the small momentum expansion of the cross-section given by eq.…”

Section: Processes Involving Neutrinosmentioning

confidence: 99%

“…We assume that neutrino are non-relativistic even at sufficiently high redshift, which is a good approximation for z < 10 2 for m ν = 0.08 eV/c 2 . Effects of non-zero momentum on the neutrino annihilation cross-section are studied in [22,23]. Using the number density of relic neutrinos n CνB ≃ 112 cm −3 and the non-resonant cross-section in the high energy limit one can estimate the horizon for UHE neutrinos at highest energies.…”

Section: Processes Involving Neutrinosmentioning

confidence: 99%

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Cosmic absorption of ultra high energy particles

Ruffini

Vereshchagin

Xue

2016

Astrophys Space Sci

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Abstract. This paper summarizes the limits on propagation of ultra high energy particles in the Universe, set up by their interactions with cosmic background of photons and neutrinos. By taking into account cosmic evolution of these backgrounds and considering appropriate interactions we derive the mean free path for ultra high energy photons, protons and neutrinos. For photons the relevant processes are the Breit-Wheeler process as well as the double pair production process. For protons the relevant reactions are the photopion production and the Bethe-Heitler process. We discuss the interplay between the energy loss length and mean free path for the Bethe-Heitler process. Neutrino opacity is determined by its scattering off the cosmic background neutrino. We compute for the first time the high energy neutrino horizon as a function of its energy.

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Section: Processes Involving Neutrinosmentioning

confidence: 99%

Section: Processes Involving Neutrinosmentioning

confidence: 99%

Cosmic absorption of ultra high energy particles

Ruffini

Vereshchagin

Xue

2016

Astrophys Space Sci

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“…whereq · p ≡ p cos θ. The differential cross section for the resonant s-channel is [12] dσ r (E , p, s) = where s ± ≡ 2E p 2 + m 2 j ± p corresponding to head-on and parallel scattering, respectively. Eq.…”

Section: A Cross Sectionsmentioning

confidence: 99%

“…It was then considered that, at least for the lowest of the three neutrino masses, thermal effects on the CνB might be important. These were studied in detail for a single neutrino species [12], and the transmission probabilities were calculated in the context of a more realistic three-neutrino mass spectrum [13].…”

Section: Introductionmentioning

confidence: 99%

Ultra high energy neutrinos: absorption, thermal effects and signatures

Lunardini¹,

Sabancilar²,

Yang³

2013

J. Cosmol. Astropart. Phys.

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We study absorption of ultra high energy neutrinos by the cosmic neutrino background, with full inclusion of the effect of the thermal distribution of the background on the resonant annihilation channel. For a hierarchical neutrino mass spectrum (with at least one neutrino with mass below ∼ 10 −2 eV), thermal effects are important for ultra high energy neutrino sources at z > ∼ 16. The neutrino transmission probability shows no more than two separate suppression dips since the two lightest mass eigenstates contribute as a single species when thermal effects are included. Results are applied to a number of models of ultra high energy neutrino emission. Suppression effects are strong for sources that extend beyond z ∼ 10, which can be realized for certain top down scenarios, such as superheavy dark matter decays, cosmic strings and cosmic necklaces. For these, a broad suppression valley should affect the neutrino spectrum at least in the energy interval 10 12 − 10 13 GeV -which therefore is disfavored for ultra high energy neutrino searches -with only a mild dependence on the neutrino mass spectrum and hierarchy. The observation of absorption effects would indicate a population of sources beyond z ∼ 10, and favor top-down mechanisms; it would also be an interesting probe of the physics of the relic neutrino background in the unexplored redshift interval z ∼ 10 − 100.1 After neutrino decoupling, T is actually defined by Eq. (2.5).

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“…As for detailed theoretical analyses on the CνB spectroscopy using ultra-high energy cosmic rays, refer to the papers by Barenboim et al [42] and by D'Olivo et al [43]. A detailed theoretical analysis on the Z-burst can be found, for example, in the paper by Fargion et al [44].…”

Section: Cosmic Rays-cνb Scatteringmentioning

confidence: 99%

Looking for cosmic neutrino background

Yanagisawa

2014

Front. Physics

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Since the discovery of neutrino oscillation in atmospheric neutrinos by the Super-Kamiokande experiment in 1998, study of neutrinos has been one of exciting fields in high-energy physics. All the mixing angles were measured. Quests for (1) measurements of the remaining parameters, the lightest neutrino mass, the CP violating phase(s), and the sign of mass splitting between the mass eigenstates m 3 and m 1 , and (2) better measurements to determine whether the mixing angle θ 23 is less than π/4, are in progress in a well-controlled manner. Determining the nature of neutrinos, whether they are Dirac or Majorana particles is also in progress with continuous improvement. On the other hand, although the ideas of detecting cosmic neutrino background have been discussed since 1960s, there has not been a serious concerted effort to achieve this goal. One of the reasons is that it is extremely difficult to detect such low energy neutrinos from the Big Bang. While there has been tremendous accumulation of information on Cosmic Microwave Background since its discovery in 1965, there is no direct evidence for Cosmic Neutrino Background. The importance of detecting Cosmic Neutrino Background is that, although detailed studies of Big Bang Nucleosynthesis and Cosmic Microwave Background give information of the early Universe at ∼a few minutes old and ∼300 k years old, respectively, observation of Cosmic Neutrino Background allows us to study the early Universe at ∼1 s old. This article reviews progress made in the past 50 years on detection methods of Cosmic Neutrino Background.

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UHE neutrino damping in a thermal gas of relic neutrinos

Cited by 12 publications

References 32 publications

Cosmic absorption of ultra high energy particles

Cosmic absorption of ultra high energy particles

Ultra high energy neutrinos: absorption, thermal effects and signatures

Looking for cosmic neutrino background

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