scholarly journals NUCLEAR INTERACTIONS OF COSMIC RAY HIGH ENERGY PARTICLES WITH LIQUID SCINTILLATOR

1963 ◽  
Vol 19 (4) ◽  
pp. 205
Author(s):  
WANG SHIH-WEI ◽  
KUANG HAO-HWAI ◽  
YUAN YU-KUEI
Keyword(s):  
Liquid Scintillator ◽  
Cosmic Ray ◽  
High Energy ◽  
Nuclear Interactions ◽  
High Energy Particles

High energy nuclear interactions in lead by cosmic ray protons at 3500 m

1956 ◽  
Vol 4 (4) ◽  
pp. 826-833 ◽  
Author(s):  
R. Giacconi ◽  
A. Lovati ◽  
A. Mura ◽  
C. Succi
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
Nuclear Interactions

Composition and spectra of primary cosmic-ray electrons and nuclei above 10 10 eV

1975 ◽  
Vol 277 (1270) ◽  
pp. 349-363 ◽  
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
Energy Spectra ◽  
Average Lifetime ◽  
Interstellar Space ◽  
Interstellar Matter ◽  
Electromagnetic Interactions ◽  
Nuclear Species ◽  
The Galaxy ◽  
High Energy Particles

Recent experiments have extended the knowledge of the flux and energy spectra of individual cosmic-ray components to much higher energies than had previously been accessible. Both electron and nuclear components show a behaviour at high energy which is unexpected, and which carries information regarding the sources and the propagation of particles between sources and observer. Electromagnetic interactions which are suffered by the electrons in interstellar space should steepen their spectrum, a steepening that would reveal the average lifetime a cosmic-ray particle spends in the galaxy. Measurements up to 1000 GeV show no such steepening. It was discovered that the composition of the nuclear species which is now measured up to 100 GeV/nucleon changes with energy. This change indicates traversal of less interstellar matter by the high energy particles than by those of lower energy. We discuss the experimental evidence and its implication.

scholarly journals Liquid scintillator composition optimization for use in ultra-high energy cosmic ray detector systems

2017 ◽  
Vol 145 ◽  
pp. 19016
Author(s):  
Dmitriy Beznosko ◽  
Ayan Batyrkhanov ◽  
Alexander Iakovlev ◽  
Khalykbek Yelshibekov
Keyword(s):  
Liquid Scintillator ◽  
Cosmic Ray ◽  
High Energy ◽  
Ultra High Energy ◽  
Composition Optimization

An exact solution of cosmic ray modulation problem in a stationary composite heliosphere model

2019 ◽  
Vol 491 (4) ◽  
pp. 5826-5842
Author(s):  
Yuriy L Kolesnyk ◽  
Boris A Shakhov ◽  
Pavol Bobik ◽  
Marian Putis
Keyword(s):  
Exact Solution ◽  
Cosmic Ray ◽  
High Energy ◽  
Physical Processes ◽  
Modern Problem ◽  
Cosmic Ray Modulation ◽  
Initial Spectrum ◽  
Particle Speed ◽  
Particle Propagation ◽  
High Energy Particles

ABSTRACT A new theoretical approach to describe the physical processes of energy particle propagation is proposed. This approach is based on the analytically iterative method for solving closed cosmic ray (CR) modulation problems, which was proposed by Shakhov and Kolesnyk. First, we have applied the approach on a simple model of the heliosphere, wherein the diffusion coefficients κ for each region of CR modulation are constants. This approach produced a very good matching of the obtained solution and also provided a numerical solution and an analytical solution. Finally, a modern problem of CR modulation in a stationary composite model of the heliosphere was considered. This model includes an environment that contains adjacent spherically symmetric regions with different modes of propagation of the solar wind (SW) speed for each layer. The CR scattering is due to different factors for each layer of the environment, as characterized by relevant κ values that simultaneously have dependence on the momentum of the particle p and the particle speed $\upsilon$, i.e. $\kappa \propto p\upsilon$. The local interstellar spectra (LISs) are given by a power-law unmodulated spectrum with the slope of the initial spectrum α, i.e. LIS ∝ p−α. An exact solution of the problem of CR modulation for low-energy particles and high-energy particles was first derived and qualitatively compared against the Voyager 1 data.

scholarly journals Selective Effects in Cosmic Rays Induced by Coulombian Interactions with Finite Temperature Plasmas

1981 ◽  
Vol 94 ◽  
pp. 365-366
Author(s):  
J. Pérez-Peraza ◽  
S. S. Trivedi
Keyword(s):  
Cosmic Rays ◽  
Energy Levels ◽  
Cosmic Ray ◽  
High Energy ◽  
Energy Losses ◽  
Deceleration Rate ◽  
Acceleration Rate ◽  
Charge States ◽  
High Energy Particles

The role of Coulombian energy losses in cosmic ray physics is generally over simplified by using the Bethe-Block formulation which does not depend explicitly on the temperature of the medium. The role of low energy particles is usually neglected, as a result of the over estimation of losses when the temperature of the medium is ignored. A deep analysis of Coulombian losses may raise the importance of these particles in the dynamics of the Galaxy. In fact, the deceleration of these particles is determined by charge interchange processes with the target ions and electrons, which energy dependence is roughly the inverse of ionisation losses. Even high energy particles may be subject to this kind of deceleration if the temperature is very high. The consideration of Coulombian losses through all energy ranges with explicit dependence on the temperature has been discussed by Perez and Lara (1979): a fully ionized medium of hydrogen has been assumed to prevail in most of cosmic ray sources. One kind of the implications is the determination of particle composition. It is claimed that a given kind of ion is preferentially accelerated or depleted depending on whether the acceleration is higher or lower than the deceleration rate at the beginning of the acceleration of thermal material. Species which undergo depletion are accelerated only if their energy is higher than that for which both rates are equated (Ec,E′c and E′c′) in such a way that only those of the hot tails of their thermal distributions are effectively accelerated. These will appear depleted relative to other species which are free accelerated because their deceleration rates at low energies are lower than the acceleration rate. It can be noted in the next figures, that if both rates would not intersect at the beginning of the acceleration, they would not join at higher energies because the acceleration rate grows faster with energy than the deceleration rate. Three arbitrary acceleration rates are used for illustration: Fermi-2nd order (αβW), Betatron or adiabatic heating (αβ2W) and shock wave acceleration (αW), where α, β and W are the efficiency, the particles velocity and the total energy per nucleon respectively. In Fig. 1 it can be seen that this selective acceleration relative to Coulombian losses is defined at different energy levels depending on the kind of acceleration involved. Since the main effect of the temperature on the losses at the beginning of the acceleration is through the local charge states of the ions, the sequence of energy losses among different species is highly assorted. This is translated in a great amount of possibilities of particle enhancements and depletions according to the temperature of the source and the kind of acceleration operating therein. If particles under go acceleration in a fully stripped state, the sequence of losses at all energy levels is such that the heavy elements are depleted in relation with the lighter ones; same is the situation, what-ever the initial charge state, for high energy particles in the range of ionisation. It may be concluded, on basis to the observational enhancement of heavy cosmic rays, that hot regions are not likely sources, and that acceleration initiates from thermal energies. On Fig. 2 it is illustrated the enhancement of Fe over 0 in solar flare conditions, on basis to the charge states as given by Jordan (1969). If α < 2.71 s−1 both elements would be depleted, whereas if α>3.45 s−1 both would be preferentially accelerated.

scholarly journals Study on the escape timescale of high-energy particles from supernova remnants through thermal X-ray properties

2020 ◽  
Vol 72 (5) ◽  
Author(s):  
Hiromasa Suzuki ◽  
Aya Bamba ◽  
Ryo Yamazaki ◽  
Yutaka Ohira
Keyword(s):  
Power Law ◽  
Supernova Remnants ◽  
Gamma Ray ◽  
Cosmic Ray ◽  
High Energy ◽  
Spectral Shape ◽  
X Ray ◽  
Galactic Cosmic Ray ◽  
High Energy Particles ◽  
Accelerated Particles

Abstract In the current decade, GeV/TeV gamma-ray observations of several supernova remnants (SNRs) have implied that accelerated particles are escaping from their acceleration sites. However, when and how they escape from the SNR vicinities are yet to be understood. Recent studies have suggested that the particle escape might develop with thermal plasma ages of the SNRs. We present a systematic study on the time evolution of particle escape using thermal X-ray properties and gamma-ray spectra using 38 SNRs associated with GeV/TeV gamma-ray emissions. We conducted spectral fittings on the gamma-ray spectra using exponential cutoff power-law and broken power-law models to estimate the exponential cutoff or the break energies, both of which are indicators of particle escape. Plots of the gamma-ray cutoff/break energies over the plasma ages show similar tendencies to those predicted by analytical/numerical calculations of particle escape under conditions in which a shock is interacting with thin interstellar medium or clouds. The particle escape timescale is estimated as ∼100 kyr from the decreasing trends of the total energy of the confined protons with the plasma age. The large dispersions of the cutoff/break energies in the data may suggest an intrinsic variety of particle escape environments. This might be the cause of the complicated Galactic cosmic ray spectral shape measured on Earth.

scholarly journals ANGULAR DISTRIBUTION OF NUCLEAR INTERACTIONS OF HIGH ENERGY COSMIC RAY PARTICLES WITH PARAFFIN

1965 ◽  
Vol 21 (5) ◽  
pp. 976
Author(s):  
KUANG HAO-HWAI ◽  
LI RU-BAI ◽  
TAN YUE-HEN ◽  
LIU YUNG-YUIH
Keyword(s):  
Angular Distribution ◽  
Cosmic Ray ◽  
High Energy ◽  
Nuclear Interactions
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