Erratum: “Parameterization of γ,e+, and Neutrino Spectra Produced byp‐pInteraction in Astronomical Environment” (ApJ, 647, 692 [2006])

Kamae, T.; Karlsson, N.; Mizuno, T.; Abe, T.; Koi, T.

doi:10.1086/513602

Cited by 268 publications

(495 citation statements)

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“…12 of Ref. [17] one can conclude that: i) the secondary spectra are slightly harder than the primary one, consistently with the energy-dependence effect discussed above; ii) the electron spectrum is slightly harder than the positron one, i.e. D/S is slightly decreasing with energy.…”

Section: B Possible Loopholes: Further Discussionsupporting

confidence: 78%

Possible causes of a rise with energy of the cosmic ray positron fraction

Serpico

2009

Phys. Rev. D

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Based on general considerations rather than model-dependent fits to specific scenarios, we argue that an increase with energy of the positron fraction in cosmic rays, suggested by several experiments at E > ∼ 7 GeV, most likely requires a primary source of electron-positron pairs. We discuss the possible alternatives, and find none of them plausible on astrophysical or particle physics grounds. Further observational ways to test different scenarios are discussed.

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Section: B Possible Loopholes: Further Discussionsupporting

confidence: 78%

Possible causes of a rise with energy of the cosmic ray positron fraction

Serpico

2009

Phys. Rev. D

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“…In constructing our custom astrophysical models we started with a model (galdef 50p 599278) that was designed to fit the EGRET measurement [87] of the diffuse mid-latitude gammas (see e.g., [88]), which is now known to be in tension with the more recent FERMI-LAT measurements [9,10]. In addition, the work [89] has also presented a more accurate parameterization of the gamma spectra arising from the decays of spallatively-produced π 0 's, which is not yet incorporated into the latest public version of GALPROP. An as-yet unreleased version of GALPROP is expected to include this and other data and may also be accommodated by a new conventional astrophysical model.…”

Section: Jhep01(2011)064mentioning

confidence: 99%

Cosmic ray anomalies from the MSSM?

Cotta

Conley

Gainer

et al. 2011

J. High Energ. Phys.

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Abstract:The recent positron excess in cosmic rays (CR) observed by the PAMELA satellite may be a signal for dark matter (DM) annihilation. When these measurements are combined with those from FERMI on the total (e + + e − ) flux and from PAMELA itself on thep/p ratio, these and other results are difficult to reconcile with traditional models of DM, including the conventional mSUGRA version of Supersymmetry even if boosts as large as 10 3−4 are allowed. In this paper, we combine the results of a previously obtained scan over a more general 19-parameter subspace of the MSSM with a corresponding scan over astrophysical parameters that describe the propagation of CR. We then ascertain whether or not a good fit to this CR data can be obtained with relatively small boost factors while simultaneously satisfying the additional constraints arising from gamma ray data. We find that a specific subclass of MSSM models where the LSP is mostly pure bino and annihilates almost exclusively into τ pairs comes very close to satisfying these requirements. The lightestτ in this set of models is found to be relatively close in mass to the LSP and is in some cases the nLSP. These models lead to a significant improvement in the overall fit to the data by an amount ∆χ 2 ∼ 1/dof in comparison to the best fit without Supersymmetry while employing boosts ∼ 100. The implications of these models for future experiments are discussed.

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“…We first compute the ν e and ν production spectra. For both flavors we use the emissivities provided in [11] (well tuned on accelerator and CR data) for projectile energies below ∼ 500 TeV, while we adopt the ones provided in [12] above that energy range. Then we account for neutrino oscillations.…”

Section: Diffuse Galactic Neutrino Spectra Obtained With Kra Modelmentioning

confidence: 99%

Interpretation of astrophysical neutrinos observed by IceCube experiment by setting Galactic and extra-Galactic spectral components

Marinelli

Gaggero

Grasso

et al. 2016

EPJ Web of Conferences

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Abstract. The last IceCube catalog of High Energy Starting Events (HESE) obtained with a livetime of 1347 days comprises 54 neutrino events equally-distributed between the three families with energies between 25 TeV and few PeVs. Considering the homogeneous flavors distribution (1:1:1) and the spectral features of these neutrinos the IceCube collaboration claims the astrophysical origin of these events with more than 5 . The spatial distribution of cited events does not show a clear correlation with known astrophysical accelerators leaving opened both the Galactic and the extra-Galactic origin interpretations. Here, we compute the neutrino diffuse emission of our Galaxy on the basis of a recently proposed phenomenological model characterized by radially-dependent cosmic-ray (CR) transport properties. We show that the astrophysical spectrum measured by IceCube experiment can be well explained adding to the diffuse Galactic neutrino flux (obtained with this new model) a extra-Galactic component derived from the astrophysical muonic neutrinos reconstructed in the Northern hemisphere. A good agreement between the expected astrophysical neutrino flux and the IceCube data is found for the full sky as well as for the Galactic plane region.

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Erratum: “Parameterization of γ,e⁺, and Neutrino Spectra Produced byp‐pInteraction in Astronomical Environment” (ApJ, 647, 692 [2006])

Cited by 268 publications

References 0 publications

Possible causes of a rise with energy of the cosmic ray positron fraction

Possible causes of a rise with energy of the cosmic ray positron fraction

Cosmic ray anomalies from the MSSM?

Interpretation of astrophysical neutrinos observed by IceCube experiment by setting Galactic and extra-Galactic spectral components

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