Chemical Composition of Cosmic Rays around the Knee Observed by the Tibet Air-Shower-Core Detector

Amenomori, M.; Bi, X. J.; Chen, D.; Cui, S. W.; Ding, L. K.; Ding, X. H.; Fan, Chao; 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.; Le, G. M.; Li, A. F.; Li, J. Y.; Lou, Y.; Lü, H.; Lu, S. L.; Meng, X. R.; Mizutani, K.; Mu, J.; Munakata, K.; Nagai, A.; Nanjo, H.; Nakamura, Masaki; Ohnishi, M.; Ohta, I.; Ouchi, T.; Ozawa, S.; Ren, J. R.; Saito, T.; Saito, T.; Sakata, M.; Sako, T. K.; 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.; 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; Zhou, X. X.

doi:10.1143/jpsjs.78sa.206

Cited by 14 publications

(18 citation statements)

References 13 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Two separate highly significant localized fractional excess regions of cosmic rays were reported in the northern hemisphere by Milagro (Abdo et al, 2008), and also by Tibet ASγ (Amenomori et al, 2007) and ARGO-YBJ Iuppa, 2011). The observation of a small scale anisotropy at multi-TeV energies was reported by IceCube, in the southern hemisphere, as well (Abbasi et al, 2011b).…”

Section: Introductionmentioning

confidence: 81%

“…In particular, using experimental techniques in the attempt to isolate relatively localized excess or deficit regions of events that overlap over the smooth global anisotropy, angular features of order 20-30 • were discovered. Two separate, highly significant, localized, fractional, excess regions of cosmic rays were reported in the Northern Hemisphere by Milagro (Abdo et al, 2008), and also by Tibet ASγ (Amenomori et al, 2007) and ARGO-YBJ Iuppa, 2011). The observation of a small scale anisotropy at multi-TeV energies was reported by IceCube, in the Southern Hemisphere, as well (Abbasi et al, 2011).…”

Section: Cosmic Rays Anisotropymentioning

confidence: 87%

“…For instance, a scenario where the large scale anisotropy is linked to diffusion of cosmic rays through the LIMF connecting the solar system to the interstellar medium outside the local interstellar cloud (where the solar system currently resides) was proposed by Amenomori et al (2007Amenomori et al ( , 2011b. This model accounts for the apparent quadrupolar contribution observed with the large scale anisotropy.…”

Section: Cosmic Rays Anisotropymentioning

confidence: 99%

“…Another model aimed to explain the origin of the TeV small scale anisotropic features, appeals to the observation that the two localized excess regions in the Morthern Hemisphere are seemingly close to the so-called Hydrogen Deflection Plane (HDP), which is the plane containing the directions of the interstellar flow and of the magnetic field upstream the heliospheric nose (Amenomori et al, 2011b). According to this model, cosmic rays propagating along the heliotail within the HDP are bent by the heliospheric magnetic field, so that two localized excess regions are formed symmetrically separated with respect to the direction of the heliotail on the HDP.…”

Section: Cosmic Rays Anisotropymentioning

confidence: 99%

See 3 more Smart Citations

Cosmic rays and stochastic magnetic reconnection in the heliotail

Desiati

Lazarían

2012

Nonlin. Processes Geophys.

View full text Add to dashboard Cite

Abstract. Galactic cosmic rays are believed to be generated by diffusive shock acceleration processes in Supernova Remnants, and the arrival direction is likely determined by the distribution of their sources throughout the Galaxy, in particular by the nearest and youngest ones. Transport to Earth through the interstellar medium is expected to affect the cosmic ray properties as well. However, the observed anisotropy of TeV cosmic rays and its energy dependence cannot be explained with diffusion models of particle propagation in the Galaxy. Within a distance of a few parsec, diffusion regime is not valid and particles with energy below about 100 TeV must be influenced by the heliosphere and its elongated tail.

show abstract

Section: Introductionmentioning

confidence: 81%

Section: Cosmic Rays Anisotropymentioning

confidence: 87%

Section: Cosmic Rays Anisotropymentioning

confidence: 99%

Section: Cosmic Rays Anisotropymentioning

confidence: 99%

See 2 more Smart Citations

Cosmic rays and stochastic magnetic reconnection in the heliotail

Desiati

Lazarían

2012

Nonlin. Processes Geophys.

View full text Add to dashboard Cite

show abstract

“…Observations in the Northern Hemisphere were reported from energies of tens to several hundreds of GeV with muon detectors (Nagashima et al, 1998;Hall et al, 1999;Munakata et al, 2010), in the one to tens of TeV energy range with various surface arrays and underground detectors (Amenomori et al, 2005(Amenomori et al, , 2006(Amenomori et al, , 2011Guillian et al, 2007;Abdo et al, 2009;Amenomori et al, 2009;Cui, 2011;Di Sciascio, 2013;de Jong, 2011;BenZvi et al, 2013;Santander et al, 2013a), up to hundreds of TeV (Aglietta et al, 2009). Recently, similar observations of a large angular scale anisotropy were reported in the Southern Hemisphere by the IceCube Observatory, in the energy range between 10 TeV and a few PeV (Abbasi et al, 2010(Abbasi et al, , 2012Aartsen et al, 2013).…”

Section: Introductionmentioning

confidence: 99%

TeV Cosmic Ray Anisotropy and the Heliospheric Magnetic Field

Desiati

Lazarían

2014

ASTRA Proc.

View full text Add to dashboard Cite

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.

show abstract

Surveys with the Cherenkov Telescope Array

Dubus

Contreras

Funk

et al. 2013

Astroparticle Physics

133

View full text Add to dashboard Cite

Surveys open up unbiased discovery space and generate legacy datasets of long-lasting value. One of the goals of imaging arrays of Cherenkov telescopes like CTA is to survey areas of the sky for faint very high energy gamma-ray (VHE) sources, especially sources that would not have drawn attention were it not for their VHE emission (e.g. the Galactic "dark accelerators"). More than half the currently known VHE sources are to be found in the Galactic Plane. Using standard techniques, CTA can carry out a survey of the region vertical bar l vertical bar <= 60 degrees, vertical bar b vertical bar <= 2 degrees in 250 h (1/4th the available time per year at one location) down to a uniform sensitivity of 3 mCrab (a "Galactic Plane survey"). CTA could also survey 1/4th of the sky down to a sensitivity of 20 mCrab in 370 h of observing time (an "all-sky survey"), which complements well the surveys by the Fermi/LAT at lower energies and extended air shower arrays at higher energies. Observations in (non-standard) divergent pointing mode may shorten the "all-sky survey" time to about 100 h with no loss in survey sensitivity. We present the scientific rationale for these surveys, their place in the multi-wavelength context, their possible impact and their feasibility. We find that the Galactic Plane survey has the potential to detect hundreds of sources. Implementing such a survey should be a major goal of CTA. Additionally, about a dozen blazars, or counterparts to Fermi/LAT sources, are expected to be detected by the all-sky survey, whose prime motivation is the search for extragalactic "dark accelerators". (C) 2012 Elsevier B.V. All rights reserved

show abstract

Chemical Composition of Cosmic Rays around the Knee Observed by the Tibet Air-Shower-Core Detector

Cited by 14 publications

References 13 publications

Cosmic rays and stochastic magnetic reconnection in the heliotail

Cosmic rays and stochastic magnetic reconnection in the heliotail

TeV Cosmic Ray Anisotropy and the Heliospheric Magnetic Field

Surveys with the Cherenkov Telescope Array

Contact Info

Product

Resources

About