Strongly Interacting Neutrinos and the Highest Energy Cosmic Rays

Domokos, G.; Kövesi‐Domokos, S.

doi:10.1103/physrevlett.82.1366

Cited by 101 publications

(94 citation statements)

References 23 publications

(18 reference statements)

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“…Since the weakness of the gravitational interaction is partially compensated by the large number of KK states and cross sections of reactions mediated by spin 2 particles are increasing rapidly with energy, it has been argued in Refs. [20] that neutrinos could initiate the observed vertical showers at the highest energies. However, the naively found growth of σ νN ∝ s 2 violates unitarity and an unitarization procedure has to applied.…”

Section: Strongly Interacting Neutrinosmentioning

confidence: 99%

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Status of particle physics solutions to the UHECR puzzle

Kachelrieß

2004

Comptes Rendus. Physique

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Abstract. The status of solutions to the ultra-high energy cosmic ray puzzle that involve particle physics beyond the standard model is reviewed. Signatures and experimental constraints are discussed for most proposals like the Z burst model and topological defects (both allowed only as subdominant contribution), supermassive dark matter (no positive evidence from its key signatures galactic anisotropy and photon dominance), strongly interacting neutrinos or new primaries (no viable models known), and violation of Lorentz invariance (possible). Résumé. Nous présentons une revue des solutions proposées en réponseà l'énigme des rayons cosmiques ultra-énergétiques, faisant intervenir la physique des particules au-delà du Modèle Standard. Nous résumons les signatures et les contraintes expérimentales pour la plupart de ces modèles tels que : la désintégration du Z et les défauts topologiques (tous deux

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Section: Strongly Interacting Neutrinosmentioning

confidence: 99%

“…Therefore, it has been speculated that the UHE primaries initiating the observed air showers are not protons, nuclei or photons but neutrinos [19,20]. However, neutrinos are in the SM deeply penetrating particles producing mainly horizontal not vertical extensive air showers (EAS).…”

Section: Neutrinos As Primaries or Messenger Particlesmentioning

confidence: 99%

Status of particle physics solutions to the UHECR puzzle

Kachelrieß

2004

Comptes Rendus. Physique

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“…For short impact parameters, partial wave unitarity is a tall 11 In what follows we only take into account KK excitations on the gravity sector without considering string recurrences of any other field. For a treatment of the latter see e.g., [254].…”

Section: B Neutrino Interactions Mediated By Gravitymentioning

confidence: 99%

“…Many scenarii with new physics beyond the electroweak scale, M EW , have been proposed, some of which increase the weak interaction cross section (see e.g., [252][253][254][255]), and hence would have observable implications. As an example of such SM extensions, we consider in the last part of this review a scenario which has generated a great deal of recent interest.…”

Section: A Everyday Weakly Interacting Neutrinosmentioning

confidence: 99%

High energy physics in the atmosphere: phenomenology of cosmic ray air showers

et al. 2004

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The properties of cosmic rays with energies above 10 6 GeV have to be deduced from the spacetime structure and particle content of the air showers which they initiate. In this review we summarize the phenomenology of these giant air showers. We describe the hadronic interaction models used to extrapolate results from collider data to ultra high energies, and discuss the prospects for insights into forward physics at the LHC. We also describe the main electromagnetic processes that govern the longitudinal shower evolution, as well as the lateral spread of particles. Armed with these two principal shower ingredients and motivation from the underlying physics, we provide an overview of some of the different methods proposed to distinguish primary species. The properties of neutrino interactions and the potential of forthcoming experiments to isolate deeply penetrating showers from baryonic cascades are also discussed. We finally venture into a terra incognita endowed with TeV-scale gravity and explore anomalous neutrino-induced showers.

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“…See also [27] and [28], and the earliest related work [29] which we are aware of. (1), as described in the text and footnotes F4-7.…”

Section: Added Notementioning

confidence: 99%

Effect of possible stronger neutrino interaction at Eνμ∼1011 GeV upon the extraction of sin2θW from the neutral-current cross section at NuTeV

Barshay¹,

Kreyerhoff²

2002

Physics Letters B

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The possibility exists that cosmic-ray neutrinos with energies of ∼ 10 20 eV interact in the atmosphere with a cross section at the millibarn level, giving rise to some of the highest-energy air showers. In a specific dynamical model which can give rise to such a cross section, we show that there can be a small effect upon the extraction of the effective value of sin 2 θW from νµ-hadron, neutral-current cross section data at NuTeV.The possibility that neutrinos, with energies of the order of 10 20 eV, have stronger interactions with hadrons than those which are given by electroweak theory, has been considered, specifically in connection with the puzzling observation of the highest energy cosmic-ray air shower events.[1, 2] Such energetic neutrinos can propagate from sources at cosmological distances (red shifts > ∼ 1), undisturbed by the cosmic microwave background radiation, which photons largely prevent protons of > ∼ 0.6 × 10 20 eV from arriving here. [3,4] Recently [5] we have explicitly calculated a σ νµ of ∼ 10 −29 cm 2 at E νµ ∼ 10 20 eV, in a specific dynamical model which involves the hypothesis of a strong, parity-conserving interaction of ν µ with a hypothetical, point-like component of a π 0 , leading to a very massive neutral lepton L, with m L ∼ 2 × 10 6 GeV. F 1 The essential physical idea is that of neutrino structure at very small distances (< 10 −18 cm), due to hadron-like coupling to L. For this m L , E νµ must reach ∼ 2 × 10 21 eV for production of real L. However, the amplitude for the diagram in Fig. (1), which involves a virtual L, results in a cross section above the electroweak σ νµ ∼ 10 −31 cm 2 , already at E νµ ∼ 10 20 eV.[5] For a somewhat smaller m L ∼ 0.3 × 10 6 GeV, the production of real L is possible for E νµ above about 0.5 × 10 20 eV, which is close to where the GZK cut-off [3,4] is located[1, 2] for protons coming from cosmological distances. In this case σ νµ can be of the order of millibarns at E νµ ∼ 10 20 eV. Then, a dip at the GZK cut-off, followed by a "bump-structure"[10] near to 10 20 eV could occur in the air-showerThe possibility of an analogous hypothetical structure (with a charged pion) for the muon, can lead to a positive-definite, unusual contribution to (gµ − 2)/2 at the level of 10 −9 , for this value of m L . [5,6] However, in addition to the squared coupling, the magnitude is rather sensitive to possible damping at the structure vertex for virtual momentum near to m L , where the integral gets its main contribution. At present, the significance of a possible experimental deviation [7] from expectation is reduced by the correction of a long-standing sign error in the calculation of a "standard" theoretical contribution. [8,9] In this paper, we consider explicitly, only neutrino, effective neutral-current couplings.

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Strongly Interacting Neutrinos and the Highest Energy Cosmic Rays

Cited by 101 publications

References 23 publications

Status of particle physics solutions to the UHECR puzzle

Status of particle physics solutions to the UHECR puzzle

High energy physics in the atmosphere: phenomenology of cosmic ray air showers

Effect of possible stronger neutrino interaction at Eνμ∼1011 GeV upon the extraction of sin2θW from the neutral-current cross section at NuTeV

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