Validation of Cosmic Ray Ionization Model CORIMIA applied for solar energetic particles and Anomalous Cosmic Rays

2016 ◽  
Author(s):  
S. Asenovski ◽  
P. Velinov ◽  
L. Mateev
Keyword(s):  
Cosmic Rays ◽  
Cosmic Ray ◽  
Energetic Particles ◽  
Solar Energetic Particles ◽  
Anomalous Cosmic Rays ◽  
Ionization Model

scholarly journals Ulysses COSPIN observations of cosmic rays and solar energetic particles from the South Pole to the North Pole of the Sun during solar maximum

2003 ◽  
Vol 21 (6) ◽  
pp. 1217-1228 ◽  
Author(s):  
R. B. McKibben ◽  
J. J. Connell ◽  
C. Lopate ◽  
M. Zhang ◽  
J. D. Anglin ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Solar Maximum ◽  
Cosmic Ray ◽  
Energetic Particles ◽  
Solar Energetic Particles ◽  
Polar Regions ◽  
The Sun ◽  
The South ◽  
The North ◽  
Inner Heliosphere

Abstract. In 2000–2001 Ulysses passed from the south to the north polar regions of the Sun in the inner heliosphere, providing a snapshot of the latitudinal structure of cosmic ray modulation and solar energetic particle populations during a period near solar maximum.  Observations from the COSPIN suite of energetic charged particle telescopes show that latitude variations in the cosmic ray intensity in the inner heliosphere are nearly non-existent near solar maximum, whereas small but clear latitude gradients were observed during the similar phase of Ulysses’ orbit near the 1994–95 solar minimum. At proton energies above ~10 MeV and extending up to >70 MeV, the intensities are often dominated by Solar Energetic Particles (SEPs) accelerated near the Sun in association with intense solar flares and large Coronal Mass Ejections (CMEs). At lower energies the particle intensities are almost constantly enhanced above background, most likely as a result of a mix of SEPs and particles accelerated by interplanetary shocks. Simultaneous high-latitude Ulysses and near-Earth observations show that most events that produce large flux increases near Earth also produce flux increases at Ulysses, even at the highest latitudes attained. Particle anisotropies during particle onsets at Ulysses are typically directed outwards from the Sun, suggesting either acceleration extending to high latitudes or efficient cross-field propagation somewhere inside the orbit of Ulysses. Both cosmic ray and SEP observations are consistent with highly efficient transport of energetic charged particles between the equatorial and polar regions and across the mean interplanetary magnetic fields in the inner heliosphere.Key words. Interplanetary physics (cosmic rays) – Solar physics, astrophysics and astronomy (energetic particles; flares and mass ejections)

scholarly journals About the Altitude Profile of the Atmospheric Cut-Off of Cosmic Rays: New Revised Assessment

Solar Physics ◽  
2021 ◽  
Vol 296 (8) ◽  
Author(s):  
Alexander Mishev ◽  
Stepan Poluianov
Keyword(s):  
Cosmic Rays ◽  
Neutron Monitor ◽  
Cosmic Ray ◽  
High Energy ◽  
Energetic Particles ◽  
Solar Energetic Particles ◽  
Global Network ◽  
Joint Analysis ◽  
Cosmic Ray Intensity ◽  
Altitude Profile

AbstractCosmic rays, high-energy subatomic particles of extraterrestrial origin, are systematically measured by space-borne and ground-based instruments. A specific interest is paid to high-energy ions accelerated during solar eruptions, so-called solar energetic particles. In order to build a comprehensive picture of their nature, it is important to fill the gap and inter-calibrate ground-based and space-borne instruments. Here, we focus on ground-based detectors, specifically neutron monitors, which form a global network and provide continuous recording of cosmic ray intensity and its variability, used also to register relativistic solar energetic particles. The count rate of each neutron monitor is determined by the geomagnetic and atmospheric cut-offs, both being functions of the location. Here, on the basis of Monte Carlo simulations with the PLANETOCOSMICS code and by the employment of a new verified neutron monitor yield function, we assessed the atmospheric cut-off as a function of the altitude, as well as for specific stations located in the polar region. The assessed in this study altitude profile of the atmospheric cut-off for primary cosmic rays builds the basis for the joint analysis of strong solar proton events with different instruments and allows one to clarify recent definitions and related discussions about the new sub-class of events, so-called sub-ground-level enhancements (sub-GLEs).

Are Anomalous Cosmic Rays the Main Contribution to the Low-Energy Galactic Cosmic Ray Spectrum?

2008 ◽  
Vol 680 (2) ◽  
pp. L105-L108 ◽  
Author(s):  
K. Scherer ◽  
H. Fichtner ◽  
S. E. S. Ferreira ◽  
I. Büsching ◽  
M. S. Potgieter
Keyword(s):  
Cosmic Rays ◽  
Cosmic Ray ◽  
Low Energy ◽  
Anomalous Cosmic Rays ◽  
Galactic Cosmic Ray

scholarly journals On the Turbulent Reduction of Drifts for Solar Energetic Particles

2021 ◽  
Vol 922 (2) ◽  
pp. 200
Author(s):  
J. P. van den Berg ◽  
N. E. Engelbrecht ◽  
N. Wijsen ◽  
R. D. Strauss
Keyword(s):  
Pitch Angle ◽  
Cosmic Ray ◽  
Energetic Particles ◽  
Solar Energetic Particles ◽  
Particle Distributions ◽  
Magnetic Turbulence ◽  
Field Diffusion ◽  
Background Magnetic Field ◽  
Perpendicular Diffusion ◽  
Inner Heliosphere

Abstract Particle drifts perpendicular to the background magnetic field have been proposed by some authors as an explanation for the very efficient perpendicular transport of solar energetic particles (SEPs). This process, however, competes with perpendicular diffusion caused by magnetic turbulence, which can also disrupt the drift patterns and reduce the magnitude of drift effects. The latter phenomenon is well known in cosmic-ray studies, but not yet considered in SEP models. Additionally, SEP models that do not include drifts, especially for electrons, use turbulent drift reduction as a justification of this omission, without critically evaluating or testing this assumption. This article presents the first theoretical step for a theory of drift suppression in SEP transport. This is done by deriving the turbulence-dependent drift reduction function with a pitch-angle dependence, as is applicable for anisotropic particle distributions, and by investigating to what extent drifts will be reduced in the inner heliosphere for realistic turbulence conditions and different pitch-angle dependencies of the perpendicular diffusion coefficient. The influence of the derived turbulent drift reduction factors on the transport of SEPs are tested, using a state-of-the-art SEP transport code, for several expressions of theoretically derived perpendicular diffusion coefficients. It is found, for realistic turbulence conditions in the inner heliosphere, that cross-field diffusion will have the largest influence on the perpendicular transport of SEPs, as opposed to particle drifts.

Correlation analysis of solar energetic particles and secondary cosmic ray flux

2021 ◽  
Vol 75 (6) ◽  
Author(s):  
Nikola Veselinović ◽  
Mihailo Savić ◽  
Aleksandar Dragić ◽  
Dimitrije Maletić ◽  
Radomir Banjanac ◽  
...  
Keyword(s):  
Correlation Analysis ◽  
Cosmic Ray ◽  
Energetic Particles ◽  
Solar Energetic Particles ◽  
Cosmic Ray Flux

scholarly journals Impact of cosmic rays and solar energetic particles on the Earth’s ionosphere and atmosphere

2013 ◽  
Vol 3 ◽  
pp. A14 ◽  
Author(s):  
Peter I.Y. Velinov ◽  
Simeon Asenovski ◽  
Karel Kudela ◽  
Jan Lastovicka ◽  
Lachezar Mateev ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Energetic Particles ◽  
Solar Energetic Particles

scholarly journals Energetic Particles in the Local Bubble

1997 ◽  
Vol 166 ◽  
pp. 177-186 ◽  
Author(s):  
G.E. Morfill ◽  
M.J. Freyberg
Keyword(s):  
Cosmic Rays ◽  
Cosmic Ray ◽  
Energetic Particles ◽  
Current Status ◽  
Length Variation ◽  
Local Bubble ◽  
Cosmic Ray Intensity ◽  
Interstellar Clouds ◽  
Proton Intensity ◽  
Path Lengths

AbstractThe current status of observations of energetic particles in the “local bubble” is reviewed. This includes primarily “direct” measurements of cosmic rays made in the Solar System, but also the “remote sensing” made possible by observing cosmic ray produced γ-rays in the nearby interstellar clouds. Since the energetic events responsible for the formation of our local bubble may also have produced copious amounts of cosmic rays, fossil records are examined to determine whether there is a corresponding signature. The observations show that: 1) the cosmic ray (proton) intensity is fairly homogeneous throughout the local bubble and its adjacent interstellar clouds, 2) there is some evidence for a “recent” local cosmic ray injection about 40,000 years ago, 3) on longer time scales (a few million years) the cosmic ray intensity was constant within a factor two, 4) there is apparently some “activity” in the Orion cloud, as evidenced by low energy γ-ray signatures, and 5) there are two unexplained observations – the variations in the energy spectra, in particular the significantly flatter spectrum of heavy cosmic rays (Fe) and the matter path length variation, which yields consistently larger path lengths for the lighter elements (H, He). It is suggested that these observations are compatible with two cosmic ray populations – an older one in equilibrium with losses from the galaxy and a younger one which is not yet strongly affected by losses. The latter could be a cosmic ray signature of the formation of the local bubble.

scholarly journals Solar Energetic Particles (SEP) and Galactic Cosmic Rays (GCR) as tracers of solar wind conditions near Saturn: Event lists and applications

Icarus ◽  
2018 ◽  
Vol 300 ◽  
pp. 47-71 ◽  
Author(s):  
E. Roussos ◽  
C.M. Jackman ◽  
M.F. Thomsen ◽  
W.S. Kurth ◽  
S.V. Badman ◽  
...  
Keyword(s):  
Solar Wind ◽  
Cosmic Rays ◽  
Galactic Cosmic Rays ◽  
Energetic Particles ◽  
Solar Energetic Particles

scholarly journals Current status and possible extension of the global neutron monitor network

2020 ◽  
Vol 10 ◽  
pp. 17
Author(s):  
Alexander Mishev ◽  
Ilya Usoskin
Keyword(s):  
Space Weather ◽  
Neutron Monitor ◽  
Cosmic Ray ◽  
Ground Level ◽  
Solar Proton ◽  
Energetic Particles ◽  
Solar Energetic Particles ◽  
Current Status ◽  
Flight Altitude ◽  
Ground Level Enhancements

The global neutron monitor network has been successfully used over several decades to study cosmic ray variations and fluxes of energetic solar particles. Nowadays, it is used also for space weather purposes, e.g. alerts and assessment of the exposure to radiation. Here, we present the current status of the global neutron monitor network. We discuss the ability of the global neutron monitor network to study solar energetic particles, specifically during large ground level enhancements. We demonstrate as an example, the derived solar proton characteristics during ground level enhancements GLE #5 and the resulting effective dose over the globe at a typical commercial jet flight altitude of 40 kft (≈12,200 m) above sea level. We present a plan for improvement of space weather services and applications of the global neutron monitor network, specifically for studies related to solar energetic particles, namely an extension of the existing network with several new monitors. We discuss the ability of the optimized global neutron monitor network to study various populations of solar energetic particles and to provide reliable space weather services.

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