Neutrino signals in IceCube from weak production of top and charm quarks

Barger, V.; Basso, Edward; Gao, Y.; Keung, Wai-Yee

doi:10.1103/physrevd.95.093002

Cited by 11 publications

(9 citation statements)

References 43 publications

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“…Top quark production may also be accessible if enough energetic neutrinos are available. One calculation found that, for 10 PeV neutrinos, top quarks are produced in 5% of the interactions [17]. It may also be possible to study other Standard Model neutrino interactions, such as diffractive production of W bosons in the Coulomb field of oxygen nuclei [20,21]; the cross section for ν þ O → l þ W þ þ X is about 8% of the charged-current cross section for 1 PeV neutrinos.…”

Section: Discussionmentioning

confidence: 99%

“…In the relevant energy range, charm production is about 10% of the total production. Because of the quark mass, heavy quark production near its production threshold occurs at a larger average inelasticity than for light quarks at the same energy [17]. In the case of charm quarks, the inelasticity also tends to be higher even at energies far above the production threshold since they originate primarily from scattering off sea s-quarks.…”

Section: ν Interactions and Inelasticitymentioning

confidence: 99%

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Measurements using the inelasticity distribution of multi-TeV neutrino interactions in IceCube

Aartsen¹,

Anton²,

Ansseau³

et al. 2019

Phys. Rev. D

141

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Inelasticity, the fraction of a neutrino's energy transferred to hadrons, is a quantity of interest in the study of astrophysical and atmospheric neutrino interactions at multi-TeV energies with IceCube. In this work, a sample of contained neutrino interactions in IceCube is obtained from five years of data and classified as 2650 tracks and 965 cascades. Tracks arise predominantly from charged-current ν μ interactions, and we demonstrate that we can reconstruct their energy and inelasticity. The inelasticity distribution is found to be consistent with the calculation of Cooper-Sarkar et al. across the energy range from ∼1 to ∼100 TeV. Along with cascades from neutrinos of all flavors, we also perform a fit over the energy, zenith angle, and inelasticity distribution to characterize the flux of astrophysical and atmospheric neutrinos. The energy spectrum of diffuse astrophysical neutrinos is described well by a power law in both track and cascade samples, and a best-fit index γ ¼ 2.62 AE 0.07 is found in the energy range from 3.5 TeV to 2.6 PeV. Limits are set on the astrophysical flavor composition and are compatible with a ratio of ð 1 3 ∶ 1 3 ∶ 1 3 Þ ⊕. Exploiting the distinct inelasticity distribution of ν μ andν μ interactions, the atmospheric ν μ toν μ flux ratio in the energy range from 770 GeV to 21 TeV is found to be 0.77 þ0.44 −0.25 times the calculation by Honda et al. Lastly, the inelasticity distribution is also sensitive to neutrino charged-current charm production. The data are consistent with a leading-order calculation, with zero charm production excluded at 91% confidence level. Future analyses of inelasticity distributions may probe new physics that affects neutrino interactions both in and beyond the Standard Model.

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Section: Discussionmentioning

confidence: 99%

Section: ν Interactions and Inelasticitymentioning

confidence: 99%

Measurements using the inelasticity distribution of multi-TeV neutrino interactions in IceCube

Aartsen¹,

Anton²,

Ansseau³

et al. 2019

Phys. Rev. D

141

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“…It is worth mentioning that secondary lepton production (e.g., via heavy-quark production [6,60]) may also lead to an apparent starting track type event, and subsequently alter the observed inelasticity distribution. The impact of these types of contributions is best assessed by the experimental collaborations where the impact of detector response is included.…”

Section: B Inelasticity Distributionmentioning

confidence: 99%

Precise predictions for multi-TeV and PeV energy neutrino scattering rates

Gauld

2019

Phys. Rev. D

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The scattering rate of multi-TeV and PeV energy neutrinos is fast becoming an interesting topic in (astro)particle-physics. This is due to experimental progress at Neutrino Telescopes such as IceCube which have begun to gain sensitivity to the flux of neutrinos in this energy range. In view of this, a precise calculation of the scattering rate of neutrinos upon atoms is presented. The two main components of the calculation are the differential cross-section predictions for neutrino scattering upon an atomic nucleus (such as that of water), as well as upon atomic electrons. In the first case, the predictions for neutrino-nucleus cross-sections in charged-and neutral-current scattering are refined by including resonant contributions generated within the photon field of the nucleus, which alter the considered distributions by ≈ 2%. In the latter case, radiative corrections are provided for all 2 → 2 scattering processes of the formνee − → ff . For antineutrino energies of Eν e ≈ 6 PeV, where these processes become resonantly enhanced (the Glashow resonance) and dominate the total cross-section, these corrections amount to ≈ −10%. * Electronic address: r.gauld@nikhef.nl 1 Unless specifically stated, 'neutrinos' will collectively refer to both neutrinos and antineutrinos.

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“…Leptoquarks have been used to explain IceCube PeV events in Refs. [51][52][53][54][55][56]. A PeV scale supersymmetry model with gauge coupling unification, light Higgs (with fine-tuning), and PeV dark matter was introduced in [57,58].…”

Section: Introductionmentioning

confidence: 99%

Supergravity Model of Inflation and Explaining IceCube HESE Data via PeV Dark Matter Decay

Chakravarty

Khan

Mohanty

2020

Advances in High Energy Physics

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We construct a unified model of inflation and PeV dark matter with an appropriate choice of no-scale Kähler potential, superpotential, and gauge kinetic function in terms of MSSM fields and hidden sector Polonyi field. The model is consistent with the CMB observations and can explain the PeV neutrino flux observed at IceCube HESE. A Starobinsky-like Higgs-sneutrino plateau inflation is obtained from the D-term SUGRA potential while F-term being subdominant during inflation. To get PeV dark matter, SUSY breaking at PeV scale is achieved through Polonyi field. This sets the scale for soft SUSY breaking parameters m0,m1/2,A0 at the GUT scale in terms of the parameters of the model. The low-energy particle spectrum is obtained by running the RGEs. We show that the ~125 GeV Higgs and the gauge coupling unification can be obtained in this model. The 6 PeV bino-type dark matter is a subdominant fraction (~11%) of the relic density, and its decay gives the PeV scale neutrino flux observed at IceCube by appropriately choosing the couplings of the R-parity violating operators. Also, we find that there is degeneracy in scalar field parameters γ,β and coupling ζ value in producing the correct amplitude of CMB power spectrum. However, the value of parameter tanβ=1.8, which is tightly fixed from the requirement of PeV scale SUSY breaking, removes the degeneracy in the values of the scalar field parameters to provide a unique solution for inflation. In this way, it brings the explanation for dark matter, PeV neutrinos, and inflation within the same framework.

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Neutrino signals in IceCube from weak production of top and charm quarks

Cited by 11 publications

References 43 publications

Measurements using the inelasticity distribution of multi-TeV neutrino interactions in IceCube

Measurements using the inelasticity distribution of multi-TeV neutrino interactions in IceCube

Precise predictions for multi-TeV and PeV energy neutrino scattering rates

Supergravity Model of Inflation and Explaining IceCube HESE Data via PeV Dark Matter Decay

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