Properties Of Primary Cosmic Rays Research Articles

New understanding of nuclei spectra properties observed by the AMS-02 experiment

The AMS-02 experiment has observed new properties of primary cosmic rays (CRs) categorized into two groups: He-C-O-Fe and Ne-Mg-Si-S, which are independent of CR propagation. In this study, we investigate the unexpected properties of these nuclei using a spatial propagation model. All nuclei spectra are accurately reproduced and separated into primary and secondary contributions. Our findings include: 1. Primary CR spectra are identical. 2. Our calculations align with AMS-02 results for primary-dominated nuclei within a 10% difference, but show significant discrepancies for the secondary-dominated nuclei. 3. The primary element abundance at around 200 GeV is presented and compared with previous solar and Galactic results. We hope that future DAMPE experiments can provide more experimental observational evidence to validate our model calculations. Published by the American Physical Society 2024

Properties of Neon, Magnesium, and Silicon Primary Cosmic Rays Results from the Alpha Magnetic Spectrometer.

We report the observation of new properties of primary cosmic rays, neon (Ne), magnesium (Mg), and silicon (Si), measured in the rigidity range 2.15GV to 3.0TV with 1.8×10^{6} Ne, 2.2×10^{6} Mg, and 1.6×10^{6} Si nuclei collected by the Alpha Magnetic Spectrometer experiment on the International Space Station. The Ne and Mg spectra have identical rigidity dependence above 3.65GV. The three spectra have identical rigidity dependence above 86.5GV, deviate from a single power law above 200GV, and harden in an identical way. Unexpectedly, above 86.5GV the rigidity dependence of primary cosmic rays Ne, Mg, and Si spectra is different from the rigidity dependence of primary cosmic rays He, C, and O. This shows that the Ne, Mg, and Si and He, C, and O are two different classes of primary cosmic rays.

An anomaly in the properties of primary cosmic rays from the Vela cluster

Based on experimental data obtained by the GAMMA array for the knee energy region, an anomaly is found in the mass composition of primary cosmic rays arriving from the region of the Vela cluster. An original difference method is used that offers high sensitivity, protection against accidental experimental errors, and the ability to separate anomalies associated with the laboratory coordinate system from those in celestial coordinates. Allowing for the multiple scattering of charged particles in the galactic magnetic fields allows parts of the sky not directly visible from the array to be studied.

TRASGO: A proposal for a timing RPCs based detector for analyzing cosmic ray air showers

The study of the properties of primary cosmic rays with energies above 100 TeV is only accessible indirectly through the use of detector arrays at the Earth surface. Despite the extremely high multiplicity of the air showers produced in their interactions at the highest layers of the atmosphere, only a fraction of those particles arrive to the ground over surfaces from ∼0.1 to ∼100km2. The lack of information on the primary interaction and the low density of particles at the detection plane make the event by event analysis very complicated and usually only mean analysis are possible, sometimes with the help of simulation programs. The necessity of covering big surfaces to gather a significant sample of information usually leads to the use of big volume detectors with limited performances, giving only access to a small part of the information carried out by the swarm of secondary particles of the shower. In this article, we propose the development of an affordable detector, the TRASGO, based on timing RPCs (Resistive Plate Chambers) offering at the same time very good timing and tracking performances. TRASGO would allow a better and more accurate reconstruction of the air shower properties either working stand-alone or in big surface arrays.

Muon families: the breakthrough into the initial part of atmospheric cascades

Various aspects of muon families are discussed in relation to the development high energy muon detectors with a large sensitive area. Special attention is paid to the advantages of muon families compared with muon groups. The difference between muon families and gamma and hadron families is emphasised. It is shown that muon families could be a useful tool to study the initial part of atmospheric cascades and, by this means, some properties of primary cosmic rays and high energy interactions.