High-energy neutrinos from cosmic ray interactions in the local bubble

Bouyahiaoui, Makarim; Kachelrieß, M.; Semikoz, D.

doi:10.1103/physrevd.101.123023

Cited by 23 publications

(23 citation statements)

References 57 publications

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“…Similar features are also known from Nai and Hi absorption studies (Lallement et al 2014). Interaction of cosmic ray particles with the supershell may explain the highenergy neutrinos observed with IceCube (Andersen et al 2018;Bouyahiaoui et al 2020). The superbubble contains high ionisation species (Breitschwerdt & de Avillez 2006), filaments and clouds of partially neutral and possibly even molecular gas (e.g., Gry & Jenkins 2014Redfield & Linsky 2008Snowden et al 2015a;Farhang et al 2019;Linsky et al 2019) and is threaded by magnetic fields (e.g., Andersson & Potter 2006;McComas et al 2011;Frisch et al 2015;Alves et al 2018;Piirola et al 2020).…”

Section: Introductionsupporting

confidence: 73%

Can the Local Bubble explain the radio background?

Krause

Hardcastle

2021

Monthly Notices of the Royal Astronomical Society

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The ARCADE 2 balloon bolometer along with a number of other instruments have detected what appears to be a radio synchrotron background at frequencies below about 3 GHz. Neither extragalactic radio sources nor diffuse Galactic emission can currently account for this finding. We use the locally measured Cosmic ray electron population, demodulated for effects of the Solar wind, and other observational constraints combined with a turbulent magnetic field model to predict the radio synchrotron emission for the Local Bubble. We find that the spectral index of the modelled radio emission is roughly consistent with the radio background. Our model can approximately reproduce the observed antenna temperatures for a mean magnetic field strength B between 3-5 nT. We argue that this would not violate observational constraints from pulsar measurements. However, the curvature in the predicted spectrum would mean that other, so far unknown sources would have to contribute below 100 MHz. Also, the magnetic energy density would then dominate over thermal and cosmic ray electron energy density, likely causing an inverse magnetic cascade with large variations of the radio emission in different sky directions as well as high polarisation. We argue that this disagrees with several observations and thus that the magnetic field is probably much lower, quite possibly limited by equipartition with the energy density in relativistic or thermal particles (B = 0.2 − 0.6 nT). In the latter case, we predict a contribution of the Local Bubble to the unexplained radio background at most at the per cent level.

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Section: Introductionsupporting

confidence: 73%

Can the Local Bubble explain the radio background?

Krause

Hardcastle

2021

Monthly Notices of the Royal Astronomical Society

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“…The discrepancy between locally measured and the average cosmic-ray proton spectrum with the ∼2.5 slope at E > 1 TeV can be a local feature. This feature arises in the anisotropic diffusion scenario [24] in which small number of sources dominate the local cosmic-ray flux in multi-TV range [23,47,48].…”

Section: Discussionmentioning

confidence: 99%

Pion decay model of the Tibet- ASγ PeV gamma-ray signal

2021

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The Tibet-ASγ Collaboration has recently reported a measurement of diffuse γ-ray flux from the outer Galactic disk in the energy range reaching PeV. We complement this measurement with the Fermi/LAT measurement of the diffuse flux from the same sky region and study the pion decay model of the combined Fermi=LAT þ Tibet-ASγ spectrum. We find that within such a model the average cosmic-ray spectrum in the outer Galactic disk has the same characteristic features as the local cosmic-ray spectrum. In particular, it experiences a hardening at several hundred GV rigidity and a knee feature in the PV rigidity range. The slope of the average cosmic-ray spectrum above the break is close to the locally observed slope of the helium spectrum γ ≃ 2.5, but is harder than the slope of the local proton spectrum in the same rigidity range. Although the combination of Fermi/LAT and Tibet-ASγ data points to the presence of the knee in the average cosmic-ray spectrum, the quality of the data is not yet sufficient for the study of knee shape and cosmic-ray composition.

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“…the model of Ref. [15] shows where Vela accounts for the Galactic flux between 200 TeV and the second knee.…”

Section: Exponential Cut-off Break or Recovery?mentioning

confidence: 97%

Transition from Galactic to Extragalactic Cosmic Rays

Kachelrieß¹

2019

EPJ Web Conf.

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The question at which energy the transition from Galactic to extragalactic cosmic rays takes place has been a long-standing conundrum in cosmic ray physics. In the past, the transition energy has been usually associated with one of the evident features of the cosmic ray spectrum: The second knee around E≃5 ×1017 eV or the ankle at E≃3 ×1018 eV. I review anisotropy and composition data and show that they require that the transition from Galacticto extragalactic CRs has to happen early, at few ×1017 eV. As a result, a successful model for the transition should explain the ankle as a feature of the extragalactic CR spectrum. I review briefly such models and their implications.

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High-energy neutrinos from cosmic ray interactions in the local bubble

Cited by 23 publications

References 57 publications

Can the Local Bubble explain the radio background?

Can the Local Bubble explain the radio background?

Pion decay model of the Tibet- ASγ PeV gamma-ray signal

Transition from Galactic to Extragalactic Cosmic Rays

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