Method of Separating Cosmic-Ray Positrons from Electrons in the DAMPE Experiment

2022 ◽  
Author(s):  
Haoting Dai ◽  
Zang Jingjing ◽  
Ying Wang ◽  
Yunlong Zhang ◽  
Yifeng Wei ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Geomagnetic Field ◽  
Cosmic Ray ◽  
Field Of View ◽  
Particle Identification ◽  
Present Observation ◽  
Observation Data ◽  
Flight Data ◽  
The Real ◽  
Positron Flux

Abstract A method of identifying positron/electron species from the cosmic rays was studied in the DAMPE experiment. As there is no onboard magnet on the satellite, the different features imposed by the geomagnetic field on these two species were exploited for the particle identification. Application of this method to the simulation of on-orbit electrons/positrons/protons and the real flight data proves that separately measuring the CR positrons/electrons with DAMPE is feasible, though limited by the field of view for the present observation data. Further analysis on the positron flux with this method can be expected in the future.

THE ATTENUATION LENGTH OF COSMIC RAY IRON IN THE ATMOSPHERE OBTAINED BY TIGER EXPERIMENT

2005 ◽  
Vol 20 (29) ◽  
pp. 6702-6704
Author(s):  
S. KODAIRA ◽  
M. HAREYAMA ◽  
N. HASEBE ◽  
T. MIYACHI ◽  
K. SAKURAI ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Precise Measurement ◽  
Cosmic Ray ◽  
Galactic Cosmic Rays ◽  
Attenuation Length ◽  
Flight Data ◽  
Elemental Abundances ◽  
Balloon Experiment ◽  
Path Lengths ◽  
Balloon Measurements

A precise measurement of elemental abundances of galactic cosmic rays from charges Z = 20 to 34 was made by TIGER balloon experiment. Using the various path lengths in the atmosphere between 4 and 16 g/cm2 from the TIGER flight data, we derived the attenuation length of iron nuclei with the energy above 2.5 GeV/n in the atmosphere. As the result, we obtained the attenuation length of 15.5 ± 0.6 g/cm 2 which is consistent with previous results of balloon measurements.

Electron component in primary cosmic rays. II. Theory

1968 ◽  
Vol 46 (10) ◽  
pp. S533-S535
Author(s):  
A. Danjo ◽  
S. Hayakawa ◽  
F. Makino ◽  
H. Obayashi
Keyword(s):  
Cosmic Rays ◽  
Scattering Length ◽  
Cosmic Ray ◽  
Critical Energy ◽  
Galactic Cosmic Rays ◽  
Particle Diffusion ◽  
Electron Component ◽  
Positron Flux ◽  
Energy Formula ◽  
The Mean

The energy spectrum of cosmic-ray electrons can be represented by a power law with a single exponent between 3 and 50 GeV, and a break in the spectrum due to the energy loss of electrons could appear at about 50 GeV or higher. It is necessary to reconcile this high value of the critical energy [Formula: see text] with the effective thickness of matter traversed [Formula: see text] as estimated from the positron flux) and with the small amplitude of anisotropy [Formula: see text]. Hence rather severe conditions are imposed on the properties of the region in which cosmic rays are stored. We have carried out an investigation of the two-component model for storing galactic cosmic rays, which consists of disk and halo components. Assuming the intensity ratio (η) of the halo to the disk components to be nearly unity, one can assign parameters explaining various properties of cosmic rays consistently. For the case of a vanishing halo component (η = 0), the mean scattering length for particle diffusion becomes about 1018 cm.

scholarly journals Towards real-time cosmic-ray identification with the LOw Frequency ARay

2019 ◽  
Vol 216 ◽  
pp. 04005 ◽  
Author(s):  
Antonio Bonardi ◽  
Stijn Buitink ◽  
Arthur Corstanje ◽  
Heino Falcke ◽  
Brian M. Hare ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Real Time ◽  
Low Frequency ◽  
Cosmic Ray ◽  
Recognition System ◽  
Extensive Air Showers ◽  
Particle Detector ◽  
Air Showers ◽  
The Real ◽  
Radio Signals

The radio signals emitted by Extensive Air Showers have been successfully used for the last decade by LOFAR to reconstruct the properties of the primary cosmic rays. Since an effective real-time recognition system for the very short radio pulses is lacking, cosmic-ray acquisition is currently triggered by an external array of particle detector, called LORA, limiting the LOFAR collecting area to the area covered by LORA. A new algorithm for the real-time cosmic-ray detection has been developed for the LOFAR Low Band Antenna, which are sensitive between 10 and 90 MHz, and is here presented together with the latest results.

Fresh insights on properties of particle fluxes in cosmic rays measured with the Alpha Magnetic Spectrometer on the international space station

2021 ◽  
Vol 36 (12) ◽  
pp. 2130011
Author(s):  
Ziyuan Li ◽  
Jie Feng
Keyword(s):  
Cosmic Rays ◽  
Particle Physics ◽  
Space Station ◽  
Cosmic Ray ◽  
New Physics ◽  
Magnetic Spectrometer ◽  
Proton Spectrum ◽  
Momentum Dependence ◽  
Positron Flux ◽  
Alpha Magnetic Spectrometer

The Alpha Magnetic Spectrometer is a particle physics detector focusing on the search for dark matter, the existence of antimatter, the origin and composition of cosmic rays from primordial sources in the universe and the exploration of new physics in space. Important features of the elementary particle (proton, antiproton, positron and election) fluxes in cosmic rays are presented: (1) The proton spectrum has a smooth hardening from 200 GeV; (2) antiproton and positron spectra show excess from traditional physics background; (3) in particular, the positron flux shows a source term with a cutoff energy of 810 GeV, which raises the question of its source; (4) the origin of the energetic electrons is different from that of positrons and (5) the identical momentum dependence of primary and secondary cosmic ray nuclei fluxes are also reviewed.

scholarly journals Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station

2019 ◽  
Vol 209 ◽  
pp. 01007
Author(s):  
Francesco Nozzoli
Keyword(s):  
Electron Flux ◽  
Space Station ◽  
Cosmic Ray ◽  
High Energy ◽  
Precision Measurements ◽  
High Energy Electrons ◽  
Electrons And Positrons ◽  
Positron Flux ◽  
Rigidity Dependence ◽  
Alpha Magnetic Spectrometer

Precision measurements by AMS of the fluxes of cosmic ray positrons, electrons, antiprotons, protons as well as their rations reveal several unexpected and intriguing features. The presented measurements extend the energy range of the previous observations with much increased precision. The new results show that the behavior of positron flux at around 300 GeV is consistent with a new source that produce equal amount of high energy electrons and positrons. In addition, in the absolute rigidity range 60–500 GV, the antiproton, proton, and positron fluxes are found to have nearly identical rigidity dependence and the electron flux exhibits different rigidity dependence.

scholarly journals Implications of a possible TeV break in the cosmic-ray electron and positron flux

2021 ◽  
Vol 103 (11) ◽  
Author(s):  
Yu-Chen Ding ◽  
Nan Li ◽  
Chun-Cheng Wei ◽  
Yue-Liang Wu ◽  
Yu-Feng Zhou
Keyword(s):  
Cosmic Ray ◽  
Positron Flux

scholarly journals The Origin and Dynamical Effects of the Magnetic Fields and Cosmic Rays in the Disk of the Galaxy

1970 ◽  
Vol 39 ◽  
pp. 168-183
Author(s):  
E. N. Parker
Keyword(s):  
Magnetic Field ◽  
Cosmic Rays ◽  
Magnetic Fields ◽  
Dynamical Behavior ◽  
Cosmic Ray ◽  
Interested Reader ◽  
Written Text ◽  
The Galaxy ◽  
Basic Ideas ◽  
The Magnetic Field

The topic of this presentation is the origin and dynamical behavior of the magnetic field and cosmic-ray gas in the disk of the Galaxy. In the space available I can do no more than mention the ideas that have been developed, with but little explanation and discussion. To make up for this inadequacy I have tried to give a complete list of references in the written text, so that the interested reader can pursue the points in depth (in particular see the review articles Parker, 1968a, 1969a, 1970). My purpose here is twofold, to outline for you the calculations and ideas that have developed thus far, and to indicate the uncertainties that remain. The basic ideas are sound, I think, but, when we come to the details, there are so many theoretical alternatives that need yet to be explored and so much that is not yet made clear by observations.

scholarly journals Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite

2019 ◽  
Vol 5 (9) ◽  
pp. eaax3793 ◽  
Author(s):  
◽  
Q. An ◽  
R. Asfandiyarov ◽  
P. Azzarello ◽  
P. Bernardini ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Cosmic Radiation ◽  
Precise Measurement ◽  
Milky Way ◽  
Spectral Feature ◽  
Dark Matter Particle ◽  
Cosmic Ray ◽  
Galactic Cosmic Rays ◽  
Proton Spectrum ◽  
First Time

The precise measurement of the spectrum of protons, the most abundant component of the cosmic radiation, is necessary to understand the source and acceleration of cosmic rays in the Milky Way. This work reports the measurement of the cosmic ray proton fluxes with kinetic energies from 40 GeV to 100 TeV, with 2 1/2 years of data recorded by the DArk Matter Particle Explorer (DAMPE). This is the first time that an experiment directly measures the cosmic ray protons up to ~100 TeV with high statistics. The measured spectrum confirms the spectral hardening at ~300 GeV found by previous experiments and reveals a softening at ~13.6 TeV, with the spectral index changing from ~2.60 to ~2.85. Our result suggests the existence of a new spectral feature of cosmic rays at energies lower than the so-called knee and sheds new light on the origin of Galactic cosmic rays.

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