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Universe
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Solar Energetic Particles
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Solar Energetic Particles

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

Deadline for manuscript submissions: closed (28 February 2023) | Viewed by 7243

Special Issue Editor

Dr. Maria Gerontidou

E-Mail Website
Guest Editor
Physics Department, National and Kapodistrian University of Athens, 15784 Athens, Greece
Interests: cosmic ray physics; solar proton events; ground level enhancements; solar radiation; Forbush decreases; neutron monitor

Special Issue Information

Dear Colleagues,

Since the study of solar energetic particles is representative of cutting-edge space weather research, Special Issue devoted to this topic is being launched. Solar energetic particle (SEP) events are events of a pronounced increase in space particle fluxes, such as protons, electrons, and heavier ions accelerated in the Sun and moving in the interplanetary magnetic and geomagnetic field. Solar energetic particles originating from solar flares and/or coronal mass ejections with an energy ranging from tens of MeV to several GeV are of particular interest due to their effects on space weather, including radiation hazard to humans, space-borne electronic equipment, and ground-based operational systems. The duration of SPE radiation storms varies from hours to days and presents a wide-ranging energy spectrum. Therefore, a thorough understanding of the underlying physics behind the generation mechanism of SEP events and their propagation from the Sun to Earth is of great importance.

The aim of this Special Issue is to gather contributions and recent developments on the impact of solar energetic particles on space weather, their propagation through interplanetary space, and the existing and/or proposed SPE forecasting models. The issue is intended to provide a platform for scientists all over the world to promote various aspects of solar energetic particle, research introducing breakthroughs in this scientific field.

Dr. Maria Gerontidou
Guest Editor

Manuscript Submission Information

Manuscripts should be submitted online at www.mdpi.com by registering and logging in to this website. Once you are registered, click here to go to the submission form. Manuscripts can be submitted until the deadline. All submissions that pass pre-check are peer-reviewed. Accepted papers will be published continuously in the journal (as soon as accepted) and will be listed together on the special issue website. Research articles, review articles as well as short communications are invited. For planned papers, a title and short abstract (about 100 words) can be sent to the Editorial Office for announcement on this website.

Submitted manuscripts should not have been published previously, nor be under consideration for publication elsewhere (except conference proceedings papers). All manuscripts are thoroughly refereed through a single-blind peer-review process. A guide for authors and other relevant information for submission of manuscripts is available on the Instructions for Authors page. Universe is an international peer-reviewed open access monthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. Submitted papers should be well formatted and use good English. Authors may use MDPI's English editing service prior to publication or during author revisions.

Keywords

  • solar energetic particles
  • solar radiation
  • space environment forecasting models
  • coronal mass ejections
  • solar cosmic ray modulation
  • ground-level enhancements
  • space weather effects

Published Papers (5 papers)

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Research

25 pages, 954 KiB  
Article
Release Episodes of Electrons and Protons in Solar Energetic Particle Events
by Vasilis Kolympiris, Athanasios Papaioannou, Athanasios Kouloumvakos, Ioannis A. Daglis and Anastasios Anastasiadis
Universe 2023, 9(10), 432; https://doi.org/10.3390/universe9100432 - 27 Sep 2023
Viewed by 1374
Abstract
We analyzed a sample of 21 solar energetic particle (SEP) events with clear signatures in both near-relativistic electrons and high-energy protons spanning over ∼2.5 solar cycles from 1997 to 2016. We employed velocity dispersion analysis (VDA) for protons and fractional VDA (FVDA) for [...] Read more.
We analyzed a sample of 21 solar energetic particle (SEP) events with clear signatures in both near-relativistic electrons and high-energy protons spanning over ∼2.5 solar cycles from 1997 to 2016. We employed velocity dispersion analysis (VDA) for protons and fractional VDA (FVDA) for electrons, as well as time shifting analysis (TSA) in order to identify the solar release times (SRTs) of the electrons. We found that, for the majority of the events (62%), a simultaneous release was observed, while, for 14% of the events, electrons were released later than protons (i.e., delayed electrons); for 24% of the events, the opposite result was found (i.e., delayed protons). We found that the path length (L) traveled by the protons and electrons was not related to the aforementioned categorization. Moreover, we show that, in the case of simultaneous SEP events, protons and electrons are being released in close connection to type III and type II bursts, while the opposite is the case for delayed events. In addition, we demonstrate that, for the simultaneous events, both the proton and the electron release are established in heights < 5RS and that, especially for the well-connected simultaneous events, there is a co-occurrence of the type II burst with the release time of the particles. Full article
(This article belongs to the Special Issue Solar Energetic Particles)
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34 pages, 7302 KiB  
Article
Jovian Periodicities (~10 h, ~40, 20, 15 min) at ACE, Upstream from the Earth’s Bow Shock, on 25–27 November 2003
by Georgios C. Anagnostopoulos, Panagiotis K. Marhavilas, Efthymios Vassiliadis and Emmanuel T. Sarris
Universe 2023, 9(8), 357; https://doi.org/10.3390/universe9080357 - 30 Jul 2023
Viewed by 996
Abstract
It is known that Jovian radio and high energy electron emissions are observed near Earth. The question we address in this study is whether the quasi-periodic ~10 h and ~40/15–20 min (QP-10 h, QP-40/15–20 min) energetic particle and magnetic field periodicities observed by [...] Read more.
It is known that Jovian radio and high energy electron emissions are observed near Earth. The question we address in this study is whether the quasi-periodic ~10 h and ~40/15–20 min (QP-10 h, QP-40/15–20 min) energetic particle and magnetic field periodicities observed by Ulysses during its distant encounter with Jupiter in 2003 were also detectable as far as the Earth’s orbit. Surprisingly, we found that at the end of the extreme 2003 Halloween events, during times of a highly disturbed Jovian magnetosphere, as inferred from strong bKOM radio emissions observed by Ulysses, and a magnetic connection of Earth with the Jovian magnetosphere, as suggested by simulation results of the interplanetary magnetic field (IMF), the ACE satellite observed, between at least 25–27 November 2013 at the Lagrangian Point L1 (LPL1), all the characteristic Jovian periodicities. In particular, by using high-time resolution data (1/5 min), we found, for the first time, quasi-permanent electron, and magnetic field QP-10/5 h, QP-40 min and QP-15/20 data variations at LPL1 for at least three days. These observations reasonably suggest that low energy (~50–~300 keV) Jovian electrons reached the Earth’s environment; the observations examined extend the lowest energy limit of the Jovian electron spectrum from 200 keV to ~50 keV. In addition, the ACE satellite observed an impressive series of QP-10/5 h energetic (≤0.05 MeV) ion bursts (EIBs) with strong cross-field intensity gradients at the onset/decay phase of the events and energy-dependent field aligned anisotropy suggesting ion streaming in the anti-sunward direction during their main phase. A comparison of simultaneously obtained measurements by ACE at the LPL1 and by Geotail upstream from the bow shock and in the magnetosphere suggests that the QP-10/5 h EIBs are inconsistent with the concept of a terrestrial origin. On the contrary, the observations indicate that the series of QP-10/5 h EIBs on 25–27 November 2003 was a spatial effect caused by the ~10/5 h quasi-periodic approach of a large-scale sheet to the Earth’s environment. The source of the ion population forming the QP-10/5 h sharp EIBs seems most probably Jovian ions accumulated in the interplanetary space, although a solar ion contribution is possible. Based on the above results, it is reasonable to suggest that the observed QP-10 h, QP-40 min and QP-15/20 periodicities are due to Jovian influence. Further research is needed to study the cause of the QP-10/5 h EIBs. This study presents new data which extend our view on the influence of the QP-10 h/QP-40/QP-15/20 min Jovian emissions from the outer to the inner heliosphere at 1 AU. Full article
(This article belongs to the Special Issue Solar Energetic Particles)
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9 pages, 1808 KiB  
Article
Radiation Dosimetry Estimations in the Venusian Atmosphere during Different Periods of Solar Activity
by Anastasia Tezari, Argyris N. Stassinakis, Pavlos Paschalis, Helen Mavromichalaki, Christina Plainaki, Anastasios Kanellakopoulos, Norma Crosby, Mark Dierckxsens and Pantelis Karaiskos
Universe 2022, 8(12), 637; https://doi.org/10.3390/universe8120637 - 30 Nov 2022
Cited by 2 | Viewed by 1347
Abstract
The new space era has expanded the exploration of other planets of our solar system. In this work, radiation quantities are estimated in the Venusian atmosphere using the software tool DYASTIMA/DYASTIMA-R, such as the energy deposit and the ambient dose equivalent rate. Monte [...] Read more.
The new space era has expanded the exploration of other planets of our solar system. In this work, radiation quantities are estimated in the Venusian atmosphere using the software tool DYASTIMA/DYASTIMA-R, such as the energy deposit and the ambient dose equivalent rate. Monte Carlo simulations of the secondary particle cascades for different atmospheric layers were performed during solar minimum and solar maximum conditions, as well as during the extreme solar particle event that took place in October 1989, with a focus on the so-called Venusian zone of habitability. Full article
(This article belongs to the Special Issue Solar Energetic Particles)
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18 pages, 3505 KiB  
Article
Solar Energetic Particle Events and Forbush Decreases Driven by the Same Solar Sources
by Anatoly Belov, Nataly Shlyk, Maria Abunina, Elena Belova, Artem Abunin and Athanasios Papaioannou
Universe 2022, 8(8), 403; https://doi.org/10.3390/universe8080403 - 01 Aug 2022
Cited by 1 | Viewed by 1181
Abstract
The characteristics of Forbush decreases (FDs) and solar energetic particle (SEP) events driven by the same solar source (i.e., coronal mass ejection and associated solar flare) are investigated. The part of the solar disk (04∘ E–35∘ W) in which most of [...] Read more.
The characteristics of Forbush decreases (FDs) and solar energetic particle (SEP) events driven by the same solar source (i.e., coronal mass ejection and associated solar flare) are investigated. The part of the solar disk (04∘ E–35∘ W) in which most of the solar events lead both to an FD and SEP event on Earth was chosen. SEPs for different energies (E > 10 MeV, E > 100 MeV, and Ground Level Enhancements) and with different flux thresholds were considered independently. The obtained results were compared with the control group of FDs that had solar sources within the same longitudinal zone but were not accompanied by any SEPs. It is shown that coronal mass ejections (CMEs) followed by SEPs have a very high probability of creating a large FD in the Earth’s orbit and to further cause a geomagnetic storm. It is also found that the accelerative and modulating efficiencies of powerful solar events are well correlated; this can be explained mostly by high speeds of the corresponding CMEs. Full article
(This article belongs to the Special Issue Solar Energetic Particles)
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12 pages, 6779 KiB  
Article
The Updated Version of the A.Ne.Mo.S. GLE Alert System: The Case of the Ground-Level Enhancement GLE73 on 28 October 2021
by Helen Mavromichalaki, Pavlos Paschalis, Maria Gerontidou, Maria-Christina Papailiou, Evangelos Paouris, Anastasia Tezari, Dimitra Lingri, Maria Livada, Argyris N. Stassinakis, Norma Crosby and Mark Dierckxsens
Universe 2022, 8(7), 378; https://doi.org/10.3390/universe8070378 - 11 Jul 2022
Cited by 4 | Viewed by 1378
Abstract
A ground-level enhancement (GLE) event is a sudden increase in cosmic ray intensity originated by solar sources and recorded by ground-based detectors. GLEs are invariably associated with large solar flares that can release and accelerate solar particles at high energies. The minimum kinetic [...] Read more.
A ground-level enhancement (GLE) event is a sudden increase in cosmic ray intensity originated by solar sources and recorded by ground-based detectors. GLEs are invariably associated with large solar flares that can release and accelerate solar particles at high energies. The minimum kinetic energy of particles reaching the Earth’s surface is >433 MeV at sea level and about 300 MeV/n at high-mountain altitude of about 3000 m a.s.l. Even though these abrupt events linked to solar activity are quite rare, they can have a great impact on technological systems and human health when recorded. Therefore, the accurate and effective prognosis of such events is of great importance. In this paper, an overview of the most recently recorded GLE event and the first of solar cycle 25, i.e., GLE73, as well as a post-event analysis is presented. GLE73 was detected on 28 October 2021 and was associated with the active region AR12887 on the central part of the solar disk, which produced an X1.0 solar flare. The event was registered by several stations of the worldwide ground-based neutron monitor network. An accurate alert was issued successfully by the ESA R-ESC federated product GLE Alert Plus, as well as the updated GLE Alert++ System of the Athens Neutron Monitor Station (A.Ne.Mo.S.). It should be emphasized that the GLE Alert++ signal by NKUA/A.Ne.Mo.S. was issued 45 min earlier than the one issued by GOES. A short description and the advantages of this last system are provided. Full article
(This article belongs to the Special Issue Solar Energetic Particles)
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