TeV Cosmic Ray Anisotropy and the Heliospheric Magnetic Field

Desiati, P.; Lazarían, A.

doi:10.5194/ap-1-65-2014

Cited by 3 publications

(3 citation statements)

References 45 publications

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“…Since the prediction of conventional atmospheric neutrinos from Honda et al (2007) is based on the standard US atmosphere, the expectation is corrected for annual temperature fluctuations. This is done using the formalism reported in Desiati et al (2014) and data measured by the instrument AIRS installed on the AQUA satellite (AIRS Science Team/Joao Texeira 2013). The effect of this correction is estimated to be of the order of 2% with an uncertainty of about 0.1%.…”

Section: Atmospheric Flux Uncertaintiesmentioning

confidence: 99%

Observation and Characterization of a Cosmic Muon Neutrino Flux From the Northern Hemisphere Using Six Years of Icecube Data

Aartsen¹,

Abraham²,

Ackermann³

et al. 2016

ApJ

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462

664

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The IceCube Collaboration has previously discovered a high-energy astrophysical neutrino flux using neutrino events with interaction vertices contained within the instrumented volume of the IceCube detector. We present a complementary measurement using charged current muon neutrino events where the interaction vertex can be outside this volume. As a consequence of the large muon range the effective area is significantly larger but the field of view is restricted to the Northern Hemisphere. IceCube data from 2009 through 2015 have been analyzed using a likelihood approach based on the reconstructed muon energy and zenith angle. At the highest neutrino energies between and a significant astrophysical contribution is observed, excluding a purely atmospheric origin of these events at significance. The data are well described by an isotropic, unbroken power-law flux with a normalization at neutrino energy of and a hard spectral index of . The observed spectrum is harder in comparison to previous IceCube analyses with lower energy thresholds which may indicate a break in the astrophysical neutrino spectrum of unknown origin. The highest-energy event observed has a reconstructed muon energy of which implies a probability of less than for this event to be of atmospheric origin. Analyzing the arrival directions of all events with reconstructed muon energies above no correlation with known γ-ray sources was found. Using the high statistics of atmospheric neutrinos we report the current best constraints on a prompt atmospheric muon neutrino flux originating from charmed meson decays which is below 1.06 in units of the flux normalization of the model in Enberg et al.

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Section: Atmospheric Flux Uncertaintiesmentioning

confidence: 99%

Observation and Characterization of a Cosmic Muon Neutrino Flux From the Northern Hemisphere Using Six Years of Icecube Data

Aartsen¹,

Abraham²,

Ackermann³

et al. 2016

ApJ

Self Cite

462

664

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“…In addition to this muon intensity displays a seasonal variation correlated with the temperature variations in the upper atmosphere, this was first postulated in 1952 [10]. High energy muon observations display a positive temperature dependence [11,12], where as low energy muon observations show a negative temperature dependence.…”

Section: Introductionmentioning

confidence: 84%

Atmospheric temperature dependence of muon intensity measured by the GRAPES-3 experiment

Paul¹,

Ahmad²,

Chandra³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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The large area (560 m 2 ) GRAPES-3 tracking muon telescope located at Ooty, India has been operating uninterruptedly since 2001. Everyday it records 4 × 10 9 muons of energy > 1 GeV with an angular resolution of ∼ 4 • . Atmospheric temperature variation affects the rate of decay of these GeV muons produced by the galactic cosmic rays (GCRs), which in turn modulates the intensity of detected muons. Since the daily temperature induced variation combines with the diurnal modulation of the GCRs by the magnetized solar wind, it becomes rather difficult to segregate the respective contributions of these two phenomena. A small seasonal variation in the intensity of cosmic ray muon (∼ 0.4%) with periodicity ∼ 1 year (Yr) was measured by analyzing the GRAPES-3 data of six years (2005)(2006)(2007)(2008)(2009)(2010). The effective temperature 'T eff ' of the upper atmosphere above Ooty also displayed a similar periodic variation with an amplitude of ∼ 1K, which was responsible for the observed seasonal variation in the muon intensity. At GeV energies, the muons detected by the GRAPES-3 show an anti-correlation with T eff calculated by using a hadronic attenuation length λ . Using the fast Fourier transform (FFT) technique and making use of the anti-correlation between the seasonal variation of T eff with the muon intensity, we calculated the temperature coefficient α T . The magnitude of α T was found to scale with the assumed attenuation length λ , which we varied within a range of 80-180 gcm −2 . However, the actual magnitude of the correction was found to be independent of the value of λ .

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“…These high energies are not taken under consideration here. * Corresponing author A few explanations have been proposed, either related to interstellar magnetic field variations (Amenomori et al, 2011), intermediate turbulence (Biermann et al, 2015) due to the heliotail (Desiati and Lazarian, 2014;Zhang et al, 2014;Pogorelov et al, 2015;Schwadron et al, 2015). A detailed analysis of the power spectrum is discussed in Ahlers and Mertsch (2015) where thet authors showed that the strength of the power spectrum is related to the diffusion tensor.…”

Section: Introductionmentioning

confidence: 99%

Comic ray flux anisotropies caused by astrospheres

Scherer

Strauss

Ferreira

et al. 2016

Astroparticle Physics

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Huge astrospheres or stellar wind bubbles influence the propagation of cosmic rays at energies up to the TeV range and can act as small-scale sinks decreasing the cosmic ray flux. We model such a sink (in 2D) by a sphere of radius 10\,pc embedded within a sphere of a radius of 1\,kpc. The cosmic ray flux is calculated by means of backward stochastic differential equations from an observer, which is located at $r_{0}$, to the outer boundary. It turns out that such small-scale sinks can influence the cosmic ray flux at the observer's location by a few permille (i.e\ a few 0.1\%), which is in the range of the observations by IceCube, Milagro and other large area telescopes.Comment: 10 pages, 4 Figure

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TeV Cosmic Ray Anisotropy and the Heliospheric Magnetic Field

Cited by 3 publications

References 45 publications

Observation and Characterization of a Cosmic Muon Neutrino Flux From the Northern Hemisphere Using Six Years of Icecube Data

Observation and Characterization of a Cosmic Muon Neutrino Flux From the Northern Hemisphere Using Six Years of Icecube Data

Atmospheric temperature dependence of muon intensity measured by the GRAPES-3 experiment

Comic ray flux anisotropies caused by astrospheres

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