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Journal articles on the topic 'Solar energetic particles'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 August 2024

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1

KIRÁLY, PÉTER. "SOLAR ENERGETIC PARTICLES." International Journal of Modern Physics A 20, no. 29 (2005): 6634–41. http://dx.doi.org/10.1142/s0217751x05029678.

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Energetic particles recorded in the Earth environment and in interplanetary space have a multitude of origins, i.e. acceleration and propagation histories. At early days practically all sufficiently energetic particles were considered to have come either from solar flares or from interstellar space. Later on, co-rotating interplanetary shocks, the termination shock of the supersonic solar wind, planetary bow shocks and magnetospheres, and also coronal mass ejections (CME) were recognized as energetic particle sources. It was also recognized that less energetic (suprathermal) particles of solar

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Vilmer, Nicole. "Solar flares and energetic particles." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 370, no. 1970 (2012): 3241–68. http://dx.doi.org/10.1098/rsta.2012.0104.

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Solar flares are now observed at all wavelengths from γ -rays to decametre radio waves. They are commonly associated with efficient production of energetic particles at all energies. These particles play a major role in the active Sun because they contain a large amount of the energy released during flares. Energetic electrons and ions interact with the solar atmosphere and produce high-energy X-rays and γ -rays. Energetic particles can also escape to the corona and interplanetary medium, produce radio emissions (electrons) and may eventually reach the Earth's orbit. I shall review here the av

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3

Hofer, M. Y., R. G. Marsden, T. R. Sanderson, and C. Tranquille. "From the Sun’s south to the north pole – Ulysses COSPIN/LET composition measurements at solar maximum." Annales Geophysicae 21, no. 6 (2003): 1383–91. http://dx.doi.org/10.5194/angeo-21-1383-2003.

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Abstract. Based on elemental abundance ratios derived from the Ulysses COSPIN/LET measurements, we classified the energetic particle populations during and after the socalled Fast Latitude Scan – the time period during which the Ulysses spacecraft traveled from the highest heliolatitude south to maximum northern latitude, i.e. 27 November 2000 to 13 October 2001 – as being mixed between solar energetic particles (major component) and particles accelerated at stream interaction regions. During the fast latitude scan, the Ulysses spacecraft made the first transit in heliolatitude from pole to po

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4

Dröge, Wolfgang. "Transport of Solar Energetic Particles." International Astronomical Union Colloquium 142 (1994): 567–76. http://dx.doi.org/10.1017/s0252921100077824.

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AbstractNew developments in the understanding of the interplanetary transport of solar cosmic rays are reviewed. Based on carefully analyzed solar particle events observed on the Helios and ISEE 3 spacecraft, the relation of transport parameters to the structure of the interplanetary magnetic field is discussed. Special emphasis is given to a comparison of particle mean free paths determined from fits to intensity and anisotropy profiles with theoretical predictions derived from magnetic field spectra measured at the time of the solar particle event. Different aspects of the turbulence and wav

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5

Wang, J. F., and G. Qin. "The Effect of Solar Wind on Charged Particles’ Diffusion Coefficients." Astrophysical Journal 961, no. 1 (2024): 6. http://dx.doi.org/10.3847/1538-4357/ad09b7.

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Abstract The transport of energetic charged particles through magnetized plasmas is ubiquitous in interplanetary space and astrophysics, and the important physical quantities are the parallel and perpendicular diffusion coefficients of energetic charged particles. In this paper, the influence of solar wind on particle transport is investigated. Using the focusing equation, we obtain parallel and perpendicular diffusion coefficients, accounting for the solar wind effect. For different conditions, the relative importance of the solar wind effect to diffusion is investigated. It is shown that, wh

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6

McKibben, R. B., J. J. Connell, C. Lopate, et al. "Ulysses COSPIN observations of cosmic rays and solar energetic particles from the South Pole to the North Pole of the Sun during solar maximum." Annales Geophysicae 21, no. 6 (2003): 1217–28. http://dx.doi.org/10.5194/angeo-21-1217-2003.

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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 minim

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7

Vlahos, Loukas, Anastasios Anastasiadis, Athanasios Papaioannou, Athanasios Kouloumvakos, and Heinz Isliker. "Sources of solar energetic particles." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 377, no. 2148 (2019): 20180095. http://dx.doi.org/10.1098/rsta.2018.0095.

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Solar energetic particles are an integral part of the physical processes related with space weather. We present a review for the acceleration mechanisms related to the explosive phenomena (flares and/or coronal mass ejections, CMEs) inside the solar corona. For more than 40 years, the main two-dimensional cartoon representing our understanding of the explosive phenomena inside the solar corona remained almost unchanged. The acceleration mechanisms related to solar flares and CMEs also remained unchanged and were part of the same cartoon. In this review, we revise the standard cartoon and prese

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8

Dröge, Wolfgang. "Particle Acceleration by Waves and Fields." Highlights of Astronomy 11, no. 2 (1998): 865–68. http://dx.doi.org/10.1017/s1539299600018967.

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The acceleration of electrons and charged nuclei to high energies is a phenomenon occuring at many sites throughout the universe, including the galaxy, pulsars, quasars, and around black holes. In the heliosphere, large solar flares and the often associated coronal mass ejections (CMEs) are the most energetic natural particle accelerators, occasionally accelerating protons to GeV and electrons to tens of MeV energies. The observation of these particles offers the unique opportunity to study fundamental processes in astrophysics. Particles that escape into interplanetary space can be observed i

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9

Poluianov, S., G. A. Kovaltsov, and I. G. Usoskin. "Solar energetic particles and galactic cosmic rays over millions of years as inferred from data on cosmogenic 26Al in lunar samples." Astronomy & Astrophysics 618 (October 2018): A96. http://dx.doi.org/10.1051/0004-6361/201833561.

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Aims. Lunar soil and rocks are not protected by a magnetic field or an atmosphere and are continuously irradiated by energetic particles that can produce cosmogenic radioisotopes directly inside rocks at different depths depending on the particle’s energy. This allows the mean fluxes of solar and galactic cosmic rays to be assessed on the very long timescales of millions of years. Methods. Here we show that lunar rocks can serve as a very good particle integral spectrometer in the energy range 20–80 MeV. We have developed a new method based on precise modeling, that is applied to measurements

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10

Droege, Wolfgang. "Transport of solar energetic particles." Astrophysical Journal Supplement Series 90 (February 1994): 567. http://dx.doi.org/10.1086/191876.

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11

Ruffolo, D. "Classification of solar energetic particles." Advances in Space Research 30, no. 1 (2002): 45–54. http://dx.doi.org/10.1016/s0273-1177(02)00177-1.

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12

Mitchell, J. G., C. M. S. Cohen, T. J. Eddy, et al. "A Living Catalog of Parker Solar Probe IS⊙IS Energetic Particle Enhancements." Astrophysical Journal Supplement Series 264, no. 2 (2023): 31. http://dx.doi.org/10.3847/1538-4365/aca4c8.

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Abstract Energetic charged particles are pervasive throughout the heliosphere with contributions from solar energetic particle events, stream and corotating interaction regions, galactic cosmic rays, anomalous cosmic rays, and suprathermal ions. The Integrated Science Investigation of the Sun (IS⊙IS) on board the Parker Solar Probe is a suite of energetic particle detectors covering the energy range ∼20 keV–200 MeV nuc−1. IS⊙IS measures energetic particles closer to the Sun than any instrument suite in history, providing a singular view of the energetic particle population in a previously unex

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13

Starkey, M. J., M. A. Dayeh, M. I. Desai, R. Bučík, S. T. Hart, and H. A. Elliott. "Multispacecraft Energetic Particle Enhancements Associated with a Single Corotating Interaction Region." Astrophysical Journal 962, no. 2 (2024): 160. http://dx.doi.org/10.3847/1538-4357/ad1cea.

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Abstract The radial evolution of particles accelerated at corotating interaction regions (CIRs) is not fully understood, particularly the distance range over which this particle acceleration occurs and how the energy spectra are modulated by transport through the inner heliosphere. Here, we present observations of energetic proton enhancements associated with a CIR observed by Parker Solar Probe on 2021 April 25 during the inbound leg of its orbit near ∼46 R s (∼0.21 au). The CIR is identified at additional spacecraft (Solar Terrestrial Relations Observatory, STEREO-A; Solar Orbiter, SolO; and

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14

Torsti, J., E. Valtonen, L. Kocharov, et al. "Energetic particle investigation using the ERNE instrument." Annales Geophysicae 14, no. 5 (1996): 497–502. http://dx.doi.org/10.1007/s00585-996-0497-5.

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Abstract. During solar flares and coronal mass ejections, nuclei and electrons accelerated to high energies are injected into interplanetary space. These accelerated particles can be detected at the SOHO satellite by the ERNE instrument. From the data produced by the instrument, it is possible to identify the particles and to calculate their energy and direction of propagation. Depending on variable coronal/interplanetary conditions, different kinds of effects on the energetic particle transport can be predicted. The problems of interest include, for example, the effects of particle properties

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Petukhov, Ivan, Anastasia Petukhova, and Stanislav Petukhov. "Formation of the Injection Function of Solar Energetic Particles in Gradual Events." Astrophysical Journal 953, no. 1 (2023): 94. http://dx.doi.org/10.3847/1538-4357/ace31f.

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Abstract We present a model for solar energetic particle injection into interplanetary space in gradual events, in which particle acceleration occurs in a limited region of the solar atmosphere. The distribution function of particles accelerated by the diffusion mechanism is calculated. The flux of injected solar energetic particles is determined as a function of time and energy. We provide an explanation of the characteristic properties of the injection function and their dependence on the particle energy. Comparing the calculation results with ground-based measurements in the 2001 April 15 e

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16

Chen, Xiaomin, and Chuan Li. "Three-stage Acceleration of Solar Energetic Particles Detected by Parker Solar Probe." Astrophysical Journal Letters 967, no. 2 (2024): L33. http://dx.doi.org/10.3847/2041-8213/ad4a79.

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Abstract Coronal mass ejections (CMEs) drive powerful shocks and thereby accelerate solar energetic particles (SEPs) as they propagate from the corona into interplanetary space. Here we present the processes of three-stage particle acceleration by a CME-driven shock detected by the in situ spacecraft—Parker Solar Probe (PSP) on 2022 August 27. The onset of SEPs is produced by a fast CME with a speed of 1284 km s−1 when it propagates to ∼2.85 R ⊙. The second stage of particle acceleration occurs when the fast CME catches up and interacts with a preceding slow one in interplanetary space at ∼40

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17

Anttila, A., and T. Sahla. "ERNE observations of energetic particles associated with Earth-directed coronal mass ejections in April and May, 1997." Annales Geophysicae 18, no. 11 (2000): 1373–81. http://dx.doi.org/10.1007/s00585-000-1373-3.

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Abstract. Two Earth-directed coronal mass ejections (CMEs), which were most effective in energetic (~1–50 MeV) particle acceleration during the first 18 months since the Solar and Heliospheric Observatory (SOHO) launch, occurred on April 7 and May 12, 1997. In the analysis of these events we have deconvoluted the injection spectrum of energetic protons by using the method described by Anttila et al. In order to apply the method developed earlier for data of a rotating satellite (Geostationary Operational Environmental Satellites, GOES), we first had to develop a method to calculate the omnidir

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18

Khabarova, Olga V., Olga E. Malandraki, Gary P. Zank, Gang Li, Jakobus A. le Roux, and Gary M. Webb. "Re-Acceleration of Energetic Particles in Large-Scale Heliospheric Magnetic Cavities." Proceedings of the International Astronomical Union 13, S335 (2017): 75–81. http://dx.doi.org/10.1017/s1743921318000285.

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AbstractCase studies show that some energetic particle flux enhancements up to MeV/nuc. observed at 1 AU cannot be treated as a consequence of particle acceleration at shocks or during flares. Atypical energetic particle events (AEPEs) are often detected during crossings of magnetic cavities formed by strong current sheets of various origins in the solar wind. Such cavities confine small-scale magnetic islands (SMIs) produced by magnetic reconnection. SMIs, in turn, trap and re-accelerate energetic particles according to predictions based on the theory of Zank et al. describing stochastic part

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19

Wang, Linghua, Gang Li, Albert Y. Shih, Robert P. Lin, and Robert F. Wimmer-Schweingruber. "SIMULATION OF ENERGETIC NEUTRAL ATOMS FROM SOLAR ENERGETIC PARTICLES." Astrophysical Journal 793, no. 2 (2014): L37. http://dx.doi.org/10.1088/2041-8205/793/2/l37.

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20

McGuire, R. E., T. T. von Rosenvinge, and F. B. McDonald. "The composition of solar energetic particles." Astrophysical Journal 301 (February 1986): 938. http://dx.doi.org/10.1086/163958.

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21

Reames, Donald V. "Energetic particles from impulsive solar flares." Astrophysical Journal Supplement Series 73 (June 1990): 235. http://dx.doi.org/10.1086/191456.

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22

Florinski, V., and J. R. Jokipii. "Solar-wind acceleration by energetic particles." Geophysical Research Letters 24, no. 19 (1997): 2383–86. http://dx.doi.org/10.1029/97gl52456.

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23

Reames, Donald V. "Solar energetic particles: A paradigm shift." Reviews of Geophysics 33 (1995): 585. http://dx.doi.org/10.1029/95rg00188.

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24

Reames, D. V., C. K. Ng, and D. Berdichevsky. "Angular Distributions of Solar Energetic Particles." Astrophysical Journal 550, no. 2 (2001): 1064–74. http://dx.doi.org/10.1086/319810.

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25

Király, Péter. "Heliospheric Magnetic Fields, Energetic Particles, and the Solar Cycle." International Astronomical Union Colloquium 179 (2000): 431–37. http://dx.doi.org/10.1017/s0252921100064976.

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AbstractThe heliosphere is the region filled with magnetized plasma of mainly solar origin. It extends from the solar corona to well beyond the planets, and is separated from the interstellar medium by the heliopause. The latter is embedded in a complex and still unexplored boundary region. The characteristics of heliospheric plasma, fields, and energetic particles depend on highly variable internal boundary conditions, and also on quasi-stationary external ones. Both galactic cosmic rays and energetic particles of solar and heliospheric origin are subject to intensity variations over individu

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26

HEBER, BERND. "ENERGETIC PARTICLES IN THE HELIOSPHERE." International Journal of Modern Physics A 20, no. 29 (2005): 6621–32. http://dx.doi.org/10.1142/s0217751x05029654.

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The heliosphere is the region around the Sun that is filled by the solar wind and its embedded magnetic field. The interaction of the supersonic solar wind with the local interstellar medium leads to a transition from supersonic to subsonic speeds at the heliospheric termination shock. The latter is regarded to be the source of the anomalous component of cosmic rays. Within the heliosphere "local" energetic particle sources, like the Sun and interplanetary shock waves contribute to the cosmic ray flux, too. At energies below a few GeV the observed galactic and anomalous cosmic ray intensities

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27

Malandraki, O. E., E. T. Sarris, and G. Tsiropoula. "Magnetic topology of coronal mass ejection events out of the ecliptic: Ulysses/HI-SCALE energetic particle observations." Annales Geophysicae 21, no. 6 (2003): 1249–56. http://dx.doi.org/10.5194/angeo-21-1249-2003.

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Abstract. Solar energetic particle fluxes (Ee > 38 keV) observed by the ULYSSES/HI-SCALE experiment are utilized as diagnostic tracers of the large-scale structure and topology of the Interplanetary Magnetic Field (IMF) embedded within two well-identified Interplanetary Coronal Mass Ejections (ICMEs) detected at 56° and 62° south heliolatitudes by ULYSSES during the solar maximum southern high-latitude pass. On the basis of the energetic solar particle observations it is concluded that: (A) the high-latitude ICME magnetic structure observed in May 2000 causes a depression in the solar energ

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28

Wijsen, N., A. Aran, J. Pomoell, and S. Poedts. "Modelling three-dimensional transport of solar energetic protons in a corotating interaction region generated with EUHFORIA." Astronomy & Astrophysics 622 (January 28, 2019): A28. http://dx.doi.org/10.1051/0004-6361/201833958.

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Aims. We introduce a new solar energetic particle (SEP) transport code that aims at studying the effects of different background solar wind configurations on SEP events. In this work, we focus on the influence of varying solar wind velocities on the adiabatic energy changes of SEPs and study how a non-Parker background solar wind can trap particles temporarily at small heliocentric radial distances (≲1.5 AU) thereby influencing the cross-field diffusion of SEPs in the interplanetary space. Methods. Our particle transport code computes particle distributions in the heliosphere by solving the fo

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Schlickeiser, Reinhard, and Ulrich Achat. "Cosmic-ray particle transport in weakly turbulent plasmas. Part 2. Mean free path of cosmic-ray protons." Journal of Plasma Physics 50, no. 1 (1993): 85–107. http://dx.doi.org/10.1017/s0022377800026933.

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We use the general Fokker–Planck coefficients derived in the first paper of this series, which describe the interaction of energetic charged particles with weak plasma turbulence in a magnetized plasma, to calculate the mean free path λ of cosmic-ray particles along the uniform background magnetic field. This quantity is a key parameter for confining energetic charged particles in cosmic plasmas, and can be experimentally inferred from interplanetary in-situ observations of solar particle events

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30

Kalegaev, Vladimir V., Natalia A. Vlasova, Ilya S. Nazarkov, and Sophia A. Melkova. "Magnetospheric access for solar protons during the January 2005 SEP event." Journal of Space Weather and Space Climate 8 (2018): A55. http://dx.doi.org/10.1051/swsc/2018040.

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The early phase of the extraordinary solar energetic particle 20 January, 2005 event having the highest peak flux of any SEP in the past 50 years of protons with energies > 100 MeV is studied. Solar energetic particles (>16 MeV) entry to the Earth’s magnetosphere on January 20, 2005 under northward interplanetary magnetic field conditions is considered based on multi-satellite data analysis and magnetic field simulation. Solar wind parameters and interplanetary magnetic field data, as well as calculations in terms of the A2000 magnetospheric magnetic field model were used to specify cond

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31

Wijsen, Nicolas, David Lario, Beatriz Sánchez-Cano, et al. "The Effect of the Ambient Solar Wind Medium on a CME-driven Shock and the Associated Gradual Solar Energetic Particle Event." Astrophysical Journal 950, no. 2 (2023): 172. http://dx.doi.org/10.3847/1538-4357/acd1ed.

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Abstract We present simulation results of a gradual solar energetic particle (SEP) event detected on 2021 October 9 by multiple spacecraft, including BepiColombo (Bepi) and near-Earth spacecraft such as the Advanced Composition Explorer (ACE). A peculiarity of this event is that the presence of a high-speed stream (HSS) affected the low-energy ion component (≲5 MeV) of the gradual SEP event at both Bepi and ACE, despite the HSS having only a modest solar wind speed increase. Using the EUHFORIA (European Heliospheric FORecasting Information Asset) magnetohydrodynamic model, we replicate the sol

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32

Rodríguez-Pacheco, J., R. F. Wimmer-Schweingruber, G. M. Mason, et al. "The Energetic Particle Detector." Astronomy & Astrophysics 642 (September 30, 2020): A7. http://dx.doi.org/10.1051/0004-6361/201935287.

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After decades of observations of solar energetic particles from space-based observatories, relevant questions on particle injection, transport, and acceleration remain open. To address these scientific topics, accurate measurements of the particle properties in the inner heliosphere are needed. In this paper we describe the Energetic Particle Detector (EPD), an instrument suite that is part of the scientific payload aboard the Solar Orbiter mission. Solar Orbiter will approach the Sun as close as 0.28 au and will provide extra-ecliptic measurements beyond ∼30° heliographic latitude during the

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Vipindas, V., Sumesh Gopinath, and T. E. Girish. "A study on the variations in long-range dependence of solar energetic particles during different solar cycles." Proceedings of the International Astronomical Union 13, S340 (2018): 47–48. http://dx.doi.org/10.1017/s1743921318001692.

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AbstractSolar Energetic Particles (SEPs) are high-energy particles ejected by the Sun which consist of protons, electrons and heavy ions having energies in the range of a few tens of keVs to several GeVs. The statistical features of the solar energetic particles (SEPs) during different periods of solar cycles are highly variable. In the present study we try to quantify the long-range dependence (or long-memory) of the solar energetic particles during different periods of solar cycle (SC) 23 and 24. For stochastic processes, long-range dependence or self-similarity is usually quantified by the

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Möbius, Eberhard. "Sources and Acceleration of Energetic Particles in Planetary Magnetospheres." International Astronomical Union Colloquium 142 (1994): 521–30. http://dx.doi.org/10.1017/s0252921100077769.

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AbstractEnergetic particles in the magnetospheres of the solar system originate from various different sources, such as the solar wind, the planetary ionospheres as well as the moons and rings of the planetary systems. Important acceleration sites are the auroral regions, the magnetotail, and the equatorial regions of the magnetospheres where electric fields, wave-particle interactions and magnetic pumping are among the major acceleration mechanisms proposed. Over the last decade mass- and charge-sensitive particle spectrometers on satellites and space probes have collected a wealth of informa

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Poquerusse, M., and P. S. McIntosh. "Type III Radio Burst Productivity of Solar Flares." International Astronomical Union Colloquium 104, no. 2 (1989): 177–80. http://dx.doi.org/10.1017/s0252921100154107.

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We study the statistical relationship between optical flares and type III radio bursts, using modern and extensive computer files. Results emerge along two main lines, concerning the physical mechanism of ejection of energetic particles, and the magnetic field geometry respectively.First, we find that type III probability of occurrence increases strongly with the brightness of a flare and its proximity to a sunspot, and with accompanying prominence activity. This suggests that Bornmann's class I and III events correspond to distinct physical phenomena, particle acceleration and magnetic expans

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Li, Xiaolei, Yuming Wang, Jingnan Guo, and Shaoyu Lyu. "Solar Energetic Particles Produced during Two Fast Coronal Mass Ejections." Astrophysical Journal Letters 928, no. 1 (2022): L6. http://dx.doi.org/10.3847/2041-8213/ac5b72.

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Abstract Two recent extremely fast coronal mass ejections (CMEs) are of particular interest. The first one originated from the southern hemisphere on 2021 October 28 and caused strong solar energetic particle (SEP) events over a wide longitude range from Earth, STEREO-A, to Mars. However, the other one, originating from the center of the Earth-viewed solar disk 5 days later, left weak SEP signatures in the heliosphere. Based on the white-light images of the CMEs from the Solar and Heliospheric Observatory (SOHO) and the Ahead Solar Terrestrial Relations Observatory (STEREO-A), in combination w

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Randol, Brent M., Errol J. Summerlin, and Jeewoo Park. "Energetic Neutral Atoms from Solar Energetic Particles due to Shocks: Inclusion of Upstream Particles." Astrophysical Journal 955, no. 1 (2023): 63. http://dx.doi.org/10.3847/1538-4357/acefcc.

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Abstract Many aspects of solar energetic particles are not well understood, including their acceleration mechanism. There has been recent interest in the potential of energetic neutral atoms (ENAs) as remote probes of solar energetic particles (SEPs) and their acceleration. The single accidental observation (in physical units) has been modeled as accelerated by a coronal mass ejection (CME)-driven shock by several authors, all of whom have assumed that the upstream component of the shock can be ignored. In this article, we relax this assumption and model the flux of ENAs at 1 au due to a CME-d

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Mishev, Alexander, and Ilya Usoskin. "Current status and possible extension of the global neutron monitor network." Journal of Space Weather and Space Climate 10 (2020): 17. http://dx.doi.org/10.1051/swsc/2020020.

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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 #

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Dalla, S., A. Balogh, S. Krucker, et al. "Delay in solar energetic particle onsets at high heliographic latitudes." Annales Geophysicae 21, no. 6 (2003): 1367–75. http://dx.doi.org/10.5194/angeo-21-1367-2003.

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Abstract. Ulysses observations have shown that solar energetic particles (SEPs) can easily reach high heliographic latitudes. To obtain information on the release and propagation of SEPs prior to their arrival at Ulysses, we analyse the onsets of nine large high-latitude particle events. We measure the onset times in several energy channels, and plot them versus inverse particle speed. This allows us to derive an experimental path length and time of release from the solar atmosphere. We repeat the procedure for near-Earth observations by Wind and SOHO. We find that the derived path lengths at

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Veselovsky, Igor S. "Solar wind and solar energetic particles: origins and effects." Proceedings of the International Astronomical Union 2, S233 (2006): 489. http://dx.doi.org/10.1017/s1743921306002535.

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Leske, R. A., R. A. Mewaldt, C. M. S. Cohen, et al. "Solar Isotopic Composition as Determined Using Solar Energetic Particles." Space Science Reviews 130, no. 1-4 (2007): 195–205. http://dx.doi.org/10.1007/s11214-007-9185-3.

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42

Zhong, Y. S., G. Qin, and S. S. Wu. "Modeling the Transport of Solar Energetic Particles in a Corotating Interaction Region." Astrophysical Journal 968, no. 2 (2024): 75. http://dx.doi.org/10.3847/1538-4357/ad3fb0.

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Abstract We present a new three-dimensional (3D) magnetohydrodynamic (MHD) model and a new 3D energetic particle transport (EPT) model. The 3D MHD model numerically solves the ideal MHD equations using the relaxing total variation diminishing scheme. In the 3D MHD simulations, we use simple boundary conditions with a high-speed flow, and we can clearly identify a corotating interaction region (CIR) with the characteristics of forward shock and reverse shock. The 3D EPT model solves the Fokker–Planck transport equation for the solar energetic particles (SEPs) using backward stochastic processes

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43

Allawi, Habeeb H. "Relationship of Soft X–Ray caused from Solar Flares and Solar Energetic Particles at Maximum of Solar cycle 24." University of Thi-Qar Journal of Science 4, no. 3 (2014): 175–78. http://dx.doi.org/10.32792/utq/utjsci/v4i3.650.

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In the current research we studied solar flares and their associated interactions of solar energetic particles (SEPs) and productive relationship with X-rays generated in these blasts. Goal of this study is to detect the correlation between soft X-rays associated with SEPs. We take into consideration rely on soft X-ray emission associated with these particles as a reference guide to keep track of these particles. In this study we used three satellites research, a satellite (ERNE) which used to detect the intensity of solar energetic particles, and this satellite belonging to the U.S. space age

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Yardley, Stephanie. "The unknown origins of solar energetic particles." Astronomy & Geophysics 63, no. 3 (2022): 3.28–3.31. http://dx.doi.org/10.1093/astrogeo/atac038.

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Abstract Stephanie Yardley explores the dangers that solar energetic particles cause to modern technology and describes the efforts to understand and predict their origin using plasma composition diagnostics.

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45

Bian, N. H., and A. Gordon Emslie. "Delay-time Distributions of Solar Energetic Particles." Astrophysical Journal 880, no. 1 (2019): 11. http://dx.doi.org/10.3847/1538-4357/ab2648.

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Vampola, A. L. "Solar cycle effects on trapped energetic particles." Journal of Spacecraft and Rockets 26, no. 6 (1989): 416–27. http://dx.doi.org/10.2514/3.26087.

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Miteva, Rositsa, Susan W. Samwel, and Vratislav Krupar. "Solar energetic particles and radio burst emission." Journal of Space Weather and Space Climate 7 (2017): A37. http://dx.doi.org/10.1051/swsc/2017035.

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Dröge, W., and Y. Y. Kartavykh. "TESTING TRANSPORT THEORIES WITH SOLAR ENERGETIC PARTICLES." Astrophysical Journal 693, no. 1 (2009): 69–74. http://dx.doi.org/10.1088/0004-637x/693/1/69.

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49

Lin, R. P. "Exploring the enigma of solar energetic particles." Eos, Transactions American Geophysical Union 75, no. 40 (1994): 457. http://dx.doi.org/10.1029/94eo01079.

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Meyer, J. P. "The baseline composition of solar energetic particles." Astrophysical Journal Supplement Series 57 (January 1985): 151. http://dx.doi.org/10.1086/191000.

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