Implication of the sidereal anisotropy of ∼5 TeV cosmic ray intensity observed with the Tibet III air shower array

Amenomori, M.; Ayabe, S.; Bi, X. J.; Chen, D.; Cui, S. W.; Danzengluobu,; Ding, L. K.; Ding, X. H.; Feng, C.; Feng, Z.; Feng, Z. Y.; Gao, X. Y.; Geng, Q. X.; Guo, H. W.; He, H. H.; He, M.; Hibino, K.; Hotta, N.; Hu, Haibing; Hu, Hongbo; Huang, J.; Huang, Q.; Jia, H. Y.; Kajino, F.; Kasahara, K.; Katayose, Y.; Kato, C.; Kawata, K.; Labaciren,; Le, G. M.; Li, A. F.; Li, J. Y.; Lou, Yu‐Qing; Lü, H.; Lu, S. L.; Meng, X. R.; Mizutani, K.; Mu, J.; Munakata, K.; Nagai, A.; Nanjo, H.; Nakamura, Masaki; Ohnishi, M.; Ohta, I.; Onuma, H.; Ouchi, T.; Ozawa, S.; Ren, J. R.; Saito, T.; Saito, Takayuki; Sakata, M.; Sako, T. K.; Sasaki, Takashi; Shibata, M.; Shirai, T.; Sugimoto, H.; Takita, M.; Tan, Y. H.; Tateyama, N.; Torii, Shoji; Tsuchiya, H.; Udo, S.; Wang, B.; Wang, H.; Wang, X.; Wang, Y. G.; Wu, H. R.; Xue, L.; Yamamoto, Y.; Yan, C. T.; Yang, X. C.; Yasue, S.; Ye, Z. H.; Yu, G. C.; Yuan, A. F.; Yuda, T.; Zhang, H. M.; Zhang, J. L.; Zhang, N. J.; Zhang, X. Y.; Zhang, Y.; Zhang, Yi; Zhaxisangzhu,; Zhou, X. X.

doi:10.1063/1.2778976

Cited by 16 publications

(6 citation statements)

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“…The transition between the two anisotropy regimes is preceded by a steady decrease of the amplitude at particle energy above 10 TeV, following an increase trend at lower energies (see Amenomori et al, 2005 for instance). The global anisotropy cannot be described with a simple dipole, but as a superposition of spherical harmonic contributions, where statistically significant small angular scale features, with amplitude of order 10 −5 -10 −4 , are also observed (Abbasi et al, 2011;Santander et al, 2013a), in agreement with similar observations in the Northern Hemisphere (Amenomori et al, 2007;Abdo et al, 2008;Bartoli et al, 2013;BenZvi et al, 2013), as shown in Fig. 1.…”

Section: Introductionsupporting

confidence: 79%

“…The fact that cosmic ray anisotropy is not a simple dipole but can be mostly explained with a superposition of a dipole and quadrupole term, seems to suggest that other transport processes might be important as well. For instance drift diffusion driven by a gradient of cosmic ray density in the local interstellar medium, producing a bi-directional anisotropy, was considered by Amenomori et al (2007) and Mizoguchi et al (2009).…”

Section: Introductionmentioning

confidence: 99%

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TeV Cosmic Ray Anisotropy and the Heliospheric Magnetic Field

Desiati

Lazarían

2014

ASTRA Proc.

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Abstract. Cosmic rays are observed to possess a small non uniform distribution in arrival direction. Such anisotropy appears to have a roughly consistent topology between tens of GeV and hundreds of TeV, with a smooth energy dependency on phase and amplitude. Above a few hundreds of TeV a sudden change in the topology of the anisotropy is observed. The distribution of cosmic ray sources in the Milky Way is expected to inject anisotropy on the cosmic ray flux. The nearest and most recent sources, in particular, are expected to contribute more significantly than others. Moreover the interstellar medium is expected to have different characteristics throughout the Galaxy, with different turbulent properties and injection scales. Propagation effects in the interstellar magnetic field can shape the cosmic ray particle distribution as well. In particular, in the 1-10 TeV energy range, they have a gyroradius comparable to the size of the Heliosphere, assuming a typical interstellar magnetic field strength of 3 µG. Therefore they are expected to be strongly affected by the Heliosphere in a manner ordered by the direction of the local interstellar magnetic field and of the heliotail. In this paper we discuss on the possibility that TeV cosmic rays arrival distribution might be significantly redistributed as they propagate through the Heliosphere.

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Section: Introductionsupporting

confidence: 79%

Section: Introductionmentioning

confidence: 99%

TeV Cosmic Ray Anisotropy and the Heliospheric Magnetic Field

Desiati

Lazarían

2014

ASTRA Proc.

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“…A quantitative description of the anisotropy as a superposition of spherical harmonics (Aartsen et al, 2016b;Abeysekara et al, 2014) shows that while most of the power is in the lowmultipole (' 6 4) terms, i.e., in the dipole, quadrupole, and octupole terms, features with smaller angular scale down to sizes of a few degrees are also present. These small-scale features have been observed in the TeV range by several experiments (Bartoli et al, 2013;Abbasi et al, 2011a;Aartsen et al, 2016b;Abeysekara et al, 2014;Amenomori et al, 2007;Abdo et al, 2008), and their relative intensity is on the order of 10 À5 -10 À4 . Given the complex nature of the anisotropy, its range from large to small angular scales, and its strong dependence on energy, it has become clear that there is no single process that can account for all observations.…”

Section: Anisotropy Of Local Cosmic Raysmentioning

confidence: 73%

Astrophysical neutrinos and cosmic rays observed by IceCube

Aartsen¹,

Ackermann²,

Adams³

et al. 2018

Advances in Space Research

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The core mission of the IceCube neutrino observatory is to study the origin and propagation of cosmic rays. IceCube, with its surface component IceTop, observes multiple signatures to accomplish this mission. Most important are the astrophysical neutrinos that are produced in interactions of cosmic rays, close to their sources and in interstellar space. IceCube is the first instrument that measures the properties of this astrophysical neutrino flux and constrains its origin. In addition, the spectrum, composition, and anisotropy of the local cosmic-ray flux are obtained from measurements of atmospheric muons and showers. Here we provide an overview of recent findings from the analysis of IceCube data, and their implications to our understanding of cosmic rays.

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“…After our standard data selection, 4.5×10 10 events are left with a modal energy of 7 TeV. For more detail of the experiment and our analysis method, refer to our separate papers (Amenomori et al, 2006(Amenomori et al, , 2007Munakata et al, 2009). We include in the systematic error the amplitude observed in the anti-sidereal time frame (364.2422 cycles/yr), because a possible seasonal change of the solar daily variation due to solar activities might produce a spurious variation in the sidereal time frame, which can be estimated by the daily variation observed in the anti-sidereal time frame.…”

Section: Analysis and Resultsmentioning

confidence: 99%

Modeling of the high-energy galactic cosmic-ray anisotropy

Amenomori

2010

Astrophys. Space Sci. Trans.

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A possible origin of the large-scale anisotropy of galactic cosmic rays at TeV energies is discussed. It can be well modeled by a superposition of the Global Anisotropy and the Midscale Anisotropy. The Global Anisotropy would be generated by galactic cosmic rays interacting with the magnetic field in the local interstellar space of scale ~2 pc surrounding the heliosphere. On the other hand, the Midscale Anisotropy, possibly caused by the modulation of galactic cosmic rays in the heliotail, is expressed as two intensity enhancements placed along the Hydrogen Deflection Plane, each symmetrically centered away from the heliotail direction. We find that the separation angle between the heliotail direction and each enhancement monotonously decreases with increasing energy in an energy range 4–30 TeV

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Implication of the sidereal anisotropy of ∼5 TeV cosmic ray intensity observed with the Tibet III air shower array

Cited by 16 publications

References 0 publications

TeV Cosmic Ray Anisotropy and the Heliospheric Magnetic Field

TeV Cosmic Ray Anisotropy and the Heliospheric Magnetic Field

Astrophysical neutrinos and cosmic rays observed by IceCube

Modeling of the high-energy galactic cosmic-ray anisotropy

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