Observation of High Energy Cosmic Rays below 1017 eV

被引：2
作者：
Bertaina, M. [1 ]
机构：
[1] Univ Turin, Dipartimento Fis Gen, I-10125 Turin, Italy
来源：
INTERNATIONAL SYMPOSIUM ON THE RECENT PROGRESS OF ULTRA-HIGH ENERGY COSMIC RAY OBSERVATION | 2011年 / 1367卷
关键词：
cosmic rays; energy spectrum; composition; anisotropy; CHERENKOV-LIGHT; CHEMICAL-COMPOSITION; HELIUM SPECTRA; PROTON; TEV; ANISOTROPY; REGION; RANGE; KNEE;
D O I：
10.1063/1.3628709
中图分类号：
O59 [应用物理学];
学科分类号：
摘要：
The shape and composition of the primary spectrum as well as the anisotropy in the arrival direction of cosmic rays are key elements to understand the origin, acceleration and propagation of the galactic radiation. A more refined generation of satellites, balloon experiments, and ground-based detectors was recently developed and operated to address such problems at energies below 10(17) eV. The general picture that comes out from their results indicate that the cosmic ray spectrum has a more complex shape than a simple smooth double power law E-gamma with a break around 3-4 x 10(15) eV. The proton spectrum seems to be softer than the other primaries in the GeV - TeV range; a significant medium and large scale anisotropy exists around 2-20 TeV. Just above the knee the spectrum shows a small concavity, and around 50-100 PeV another small but statistically significant structure.
引用
收藏
页码：23 / 28
页数：6
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