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Universe
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Solar Cosmic Rays
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Solar Cosmic Rays

A special issue of Universe (ISSN 2218-1997). This special issue belongs to the section "Solar and Stellar Physics".

Deadline for manuscript submissions: closed (31 March 2022) | Viewed by 7265

Special Issue Editor

Prof. Dr. Ruiguang Wang

E-Mail Website
Guest Editor
Experimental Physics Division, Institute of High Energy Physics, The Chinese Academy of Sciences, Beijing 100049, China
Interests: cosmic ray; solar cosmic ray; solar flare; coronal mass ejection; solar energetic particle; ground-level enhancement; neutrino oscillation; reactor neutrino experiment; liquid scintillator detector

Special Issue Information

Dear Colleagues,

A large number of studies have shown that solar cosmic ray events are closely related to solar eruptive high-energy processes, such as solar flares, coronal mass ejections, reconnection, and dynamics of solar magnetic fields. Solar energetic particles may also produce a radiation hazard in space and influence the Earth’s environment. Thus, monitoring and forecasting solar particle flux has become increasingly important. Although the study of solar cosmic rays has achieved great progress in recent decades, there are still many scientific topics to be deeply understood and explored, for example, acceleration and propagation mechanisms of solar energetic particles at the Sun and in the interplanetary medium. Today, we have large amounts of data available in different energy channels to do comprehensive studies for these unknown problems.

This Special Issue focuses on the current research status and future prospects of solar cosmic rays. Any related topics or new ideas beyond the current framework, be they theoretical, experimental, data analytical or other, are welcome.

Keywords

  • Sun
  • Solar cosmic rays
  • Solar flares
  • Coronal mass ejections
  • Solar energetic particles
  • Ground level enhancement
  • Forbush effect
  • Particle acceleration
  • Particle propagation
  • Geoeffection

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Published Papers (3 papers)

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Research

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11 pages, 3425 KiB  
Article
GeV Proton Detection in the 8 November 2000 Solar Event
by Ruiguang Wang, Zhongqiang Yu, Yuqian Ma, Linkai Ding, Qingqi Zhu, Zhiguo Yao, Xinhua Ma, Yupeng Xu and Changgen Yang
Universe 2022, 8(5), 287; https://doi.org/10.3390/universe8050287 - 20 May 2022
Viewed by 1770
Abstract
In this study, we analyze the L3 precision muon spectrometer data from November 2000. The results showed that a 4.7σ muon excess appeared at a time coincident with the solar flare of 8 November 2000. This muon excess corresponded to primary protons above [...] Read more.
In this study, we analyze the L3 precision muon spectrometer data from November 2000. The results showed that a 4.7σ muon excess appeared at a time coincident with the solar flare of 8 November 2000. This muon excess corresponded to primary protons above 40 GeV, coming from a sky cell of solid angle 0.048 sr. The probability of being a background fluctuation was estimated to be about 0.1%. It is interesting and noteworthy that an M-class solar flare may also accelerate solar protons to such high energies. Full article
(This article belongs to the Special Issue Solar Cosmic Rays)
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20 pages, 516 KiB  
Article
Solar Radio Bursts Associated with In Situ Detected Energetic Electrons in Solar Cycles 23 and 24
by Rositsa Miteva, Susan W. Samwel and Svetoslav Zabunov
Universe 2022, 8(5), 275; https://doi.org/10.3390/universe8050275 - 9 May 2022
Cited by 5 | Viewed by 2413
Abstract
The first comprehensive analysis between the in situ detected solar energetic electrons (SEEs) from ACE/EPAM satellite and remotely observed radio signatures in solar cycles (SCs) 23 and 24 (1997–2019) is presented. The identified solar origin of the SEEs (in terms of solar flares, [...] Read more.
The first comprehensive analysis between the in situ detected solar energetic electrons (SEEs) from ACE/EPAM satellite and remotely observed radio signatures in solar cycles (SCs) 23 and 24 (1997–2019) is presented. The identified solar origin of the SEEs (in terms of solar flares, SFs, and coronal mass ejections, CMEs) is associated with solar radio emission of types II, III and IV, where possible. Occurrence rates are calculated as a function of the radio wavelength, from the low corona to the interplanetary space near Earth. The tendencies of the different burst appearances with respect to SC, helio-longitude, and SEE intensity are also demonstrated. The corresponding trends of the driver (in terms of median values of the SF class and CME projected speed) are also shown. A comparison with the respective results when using solar energetic protons is presented and discussed. Full article
(This article belongs to the Special Issue Solar Cosmic Rays)
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Review

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16 pages, 4530 KiB  
Review
The Evolution of Research on Abundances of Solar Energetic Particles
by Donald V. Reames
Universe 2021, 7(8), 292; https://doi.org/10.3390/universe7080292 - 8 Aug 2021
Cited by 1 | Viewed by 2402
Abstract
Sixty years of study of energetic particle abundances have made a major contribution to our understanding of the physics of solar energetic particles (SEPs) or solar cosmic rays. An early surprise was the observation in small SEP events of huge enhancements in the [...] Read more.
Sixty years of study of energetic particle abundances have made a major contribution to our understanding of the physics of solar energetic particles (SEPs) or solar cosmic rays. An early surprise was the observation in small SEP events of huge enhancements in the isotope 3He from resonant wave–particle interactions, and the subsequent observation of accompanying enhancements of heavy ions, later found to increase 1000-fold as a steep power of the mass-to-charge ratio A/Q, right across the elements from H to Pb. These “impulsive” SEP events have been related to magnetic reconnection on open field lines in solar jets; similar processes occur on closed loops in flares, but those SEPs are trapped and dissipate their energy in heat and light. After early controversy, it was established that particles in the large “gradual” SEP events are accelerated at shock waves driven by wide, fast coronal mass ejections (CMEs) that expand broadly. On average, gradual SEP events give us a measure of element abundances in the solar corona, which differ from those in the photosphere as a classic function of the first ionization potential (FIP) of the elements, distinguishing ions and neutrals. Departures from the average in gradual SEPs are also power laws in A/Q, and fits of this dependence can determine Q values and thus estimate source plasma temperatures. Complications arise when shock waves reaccelerate residual ions from the impulsive events, but excess protons and the extent of abundance variations help to resolve these processes. Yet, specific questions about SEP abundances remain. Full article
(This article belongs to the Special Issue Solar Cosmic Rays)
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