Heavy quark currents in ultra-high energy neutrino interactions

Fiore, R.; Zoller, V. R.

doi:10.1134/s002136401202004x

Cited by 4 publications

(7 citation statements)

References 16 publications

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“…The cross sections start out close to each other, within ±5% at E ν = 10 6 GeV, then spread far apart at high energies, with σ ALLM about ∼ 1.7 times of σ BDHM and σ Soyez . Other works [61,58,62,4] also display a similar result in cross sections from different models at these energies. Another important factor in tau neutrino to tau conversion is the energy distribution of tau relative to the parent neutrino.…”

Section: Neutrino Cross Sectionsupporting

confidence: 67%

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Earth skimming tau neutrino propagation

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Section: Neutrino Cross Sectionsupporting

confidence: 67%

“…For the dipole model [58,59,60,24], the wave functions for W or Z fluctuating into a quark-antiquark pair are functions of the quark masses, wherez = 1 − z and…”

Section: Neutrino Cross Sectionmentioning

confidence: 99%

Earth skimming tau neutrino propagation

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“…As the the neutrino energy further increases, the spread in cross sections increase to a factor of ∼ 1.7 for the BDHM and Soyez approach compared to the ALLM extrapolation at 10 12 GeV. For reference, recent evaluations of the neutrino cross sections with a broader range of models [25][26][27][28] show a similar spread in cross sections at these energies. The tau flux also requires a knowledge of the energy transferred from the neutrino to the tau, namely, the distribution as a function of y ≡ (E ν − E τ )/E ν .…”

Section: Neutrino Cross Sectionsmentioning

confidence: 86%

“…Among the uncertainties in these tau neutrino flux limits or eventual observation are three elements: the uncertainty in the high energy neutrino cross section [21][22][23][24][25][26][27][28][29] required to convert the tau neutrino to the tau lepton in the Earth, the inelasticity for neutrino scattering with isoscalar nucleons (how much of the neutrino energy is transferred to the tau) and the tau electromagnetic loss [30][31][32][33][34][35] as the tau transits the remaining rock before it emerges to decay into an air shower.…”

Section: Introductionmentioning

confidence: 99%

Tau energy loss and ultrahigh energy skimming tau neutrinos

et al. 2017

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We consider propagation of high-energy earth-skimming taus produced in interactions of astrophysical tau neutrinos. For astrophysical tau neutrinos, we take generic power-law flux, E −2 and the cosmogenic flux initiated by the protons. We calculate tau energy loss in several approaches, such as dipole models and the phenomenological approach in which parametrization of the F 2 is used. We evaluate the tau neutrino charged-current cross section using the same approaches for consistency. We find that uncertainty in the neutrino cross section and in the tau energy loss partially compensate giving very small theoretical uncertainty in the emerging tau flux for distances ranging from 2 to 100 km and for the energy range between 10 6 and 10 11 GeV, focusing on energies above 10 8 GeV. When we consider uncertainties in the neutrino cross section, inelasticity in neutrino interactions and the tau energy loss, which are not correlated, i.e. they are not all calculated in the same approach, theoretical uncertainty ranges from about 30% and 60% at 10 8 GeV to about factors of 3.3 and 3.8 at 10 11 GeV for the E −2 flux and the cosmogenic flux, respectively, for the distance of 10 km rock. The spread in predictions significantly increases for much larger distances, e.g., ∼1; 000 km. Most of the uncertainty comes from the treatment of photonuclear interactions of the tau in transit through large distances. We also consider Monte Carlo calculation of the tau propagation and we find that the result for the emerging tau flux is in agreement with the result obtained using analytic approach. Our results are relevant to several experiments that are looking for skimming astrophysical taus, such as the Pierre Auger Observatory, HAWC and Ashra. We evaluate the aperture for the Auger and discuss briefly application to the other two experiments.

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“…The effects of quark masses important at low Q 2 are taken into account [28]. The linear CD BFKL description of F 2 (x, Q 2 ) (dashed line) is perfect at moderate and high Q 2 where it is indistinguishable from the solid line representing the non-linear CD BFKL results (see below).…”

Section: Bfkl and Phenomenology Of Dismentioning

confidence: 97%

Non-linear BFKL dynamics: Color screening vs. gluon fusion

2013

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A feasible mechanism of unitarization of amplitudes of deep inelastic scattering at small values of Bjorken x is the gluon fusion. However, its efficiency depends crucially on the vacuum color screening effect which accompanies the multiplication and the diffusion of BFKL gluons from small to large distances. From the fits to lattice data on field strength correlators the propagation length of perturbative gluons is R c ≃ 0.2 − 0.3 fermi. The probability to find a perturbative gluon with short propagation length at large distances is suppressed exponentially. It changes the pattern of (dif)fusion dramatically. The magnitude of the fusion effect appears to be controlled by the new dimensionless parameter ∼ R 2 c /8B, with the diffraction cone slope B standing for the characteristic size of the interaction region. It should slowly ∝ 1/ ln Q 2 decrease at large Q 2 . Smallness of the ratio R 2 c /8B makes the non-linear effects rather weak even at lowest Bjorken x available at HERA. We report the results of our studies of the non-linear BFKL equation which has been generalized to incorporate the running coupling and the screening radius R c as the infrared regulator.

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Heavy quark currents in ultra-high energy neutrino interactions

Cited by 4 publications

References 16 publications

Earth skimming tau neutrino propagation

Earth skimming tau neutrino propagation

Tau energy loss and ultrahigh energy skimming tau neutrinos

Non-linear BFKL dynamics: Color screening vs. gluon fusion

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