Relevant bibliographies by topics / Solar energetic particles / Journal articles

To see the other types of publications on this topic, follow the link: Solar energetic particles.

Journal articles on the topic 'Solar energetic particles'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 August 2024

Create a spot-on reference in APA, MLA, Chicago, Harvard, and other styles

Select a source type:

Consult the top 50 journal articles for your research on the topic 'Solar energetic particles.'

Next to every source in the list of references, there is an 'Add to bibliography' button. Press on it, and we will generate automatically the bibliographic reference to the chosen work in the citation style you need: APA, MLA, Harvard, Chicago, Vancouver, etc.

You can also download the full text of the academic publication as pdf and read online its abstract whenever available in the metadata.

Browse journal articles on a wide variety of disciplines and organise your bibliography correctly.

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

Full text

Abstract:

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 origin and pick-up ions have also a vital role in giving rise to energetic particles in interplanetary disturbances. The meaning of the term "solar energetic particles" (SEP) is now somewhat vague, but essentially it refers to particles produced in disturbances fairly directly related to solar processes. Variation of intensity fluctuations with energy and with the phase of the solar cycle will be discussed. Particular attention will be given to extremes of time variation, i.e. to very quiet periods and to large events. While quiet-time fluxes are expected to shed light on some basic coronal processes, large events dominate the fluctuation characteristics of cumulated fluence, and the change of that fluctuation with energy and with the phase of the solar cycle may also provide important clues. Mainly ISEE-3 and long-term IMP-8 data will be invoked. Energetic and suprathermal particles that may never escape into interplanetary space may play an important part in heating the corona of the sun.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 available information on energetic particles provided by X-ray/γ-ray observations, with particular emphasis on the results obtained recently by the mission Reuven Ramaty High-Energy Solar Spectroscopic Imager. I shall also illustrate how radio observations contribute to our understanding of the electron acceleration sites and to our knowledge on the origin and propagation of energetic particles in the interplanetary medium. I shall finally briefly review some recent progress in the theories of particle acceleration in solar flares and comment on the still challenging issue of connecting particle acceleration processes to the topology of the complex magnetic structures present in the corona.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 pole during solar activity maximum conditions, providing a unique opportunity to acquire energetic particle composition data over a maximum range of heliolatitudes in the inner heliosphere. At low latitudes, based on our elemental abundance analysis, we found that while solar energetic particles dominated, there were indications for particle acceleration at single compression regions in a few instances. In the high heliolatitude range the observed elemental particle compositions are mainly of the solar energetic particle type. Within the statistical errors, the observed abundance ratios were independent of latitude, and were characteristic of solar energetic particles. These observations raise an important question for the theories of particle propagation in the inner heliosphere. The daily elemental abundance ratios of S/O, Mg/O and Si/O shown here are the first measured ratios at high heliolatitudes in the energy range from 13.0 to 30.0 MeV/n.Key words. Interplanetary physics (energetic particles; interplanetary shocks) – Solar physics, astrophysics and astronomy (flares and mass ejections)

APA, Harvard, Vancouver, ISO, and other styles

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

Full text

Abstract:

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 wave models for the magnetic fluctuations are considered, including the effects resulting from the finite temperature of the plasma and of resonance broadening. It is found that a modified quasi-linear theory of particle scattering taking into account the effects of plasma waves propagating with respect to the average solar wind flow and the proper treatment of the dispersion relation at high wavenumber gives results which are in several cases in good agreement with particle observations in the interplanetary medium between 0.3 and 1 AU, indicating that quasi-linear theory is probably a good approximation to a full theory of solar particle transport. This has important implications for other astrophysical problems where quasi-linear theory is often used, such as the propagation and acceleration of Galactic cosmic rays and particle acceleration at shock waves.Subject headings: acceleration of particles — cosmic rays — interplanetary medium — MHD — solar wind — Sun: particle emission

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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, when energetic charged particles are close to the Sun, for parallel diffusion, the solar wind effect needs to be taken into account. These results are important for studying energetic charged particle transport processes in the vicinity of the Sun.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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)

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 present evidence from recent global magnetohydrodynamic simulations that support the argument that explosive phenomena will lead to the spontaneous formation of current sheets in different parts of the erupting magnetic structure. The evolution of the large-scale current sheets and their fragmentation will lead to strong turbulence and turbulent reconnection during solar flares and turbulent shocks. In other words, the acceleration mechanism in flares and CME-driven shocks may be the same, and their difference will be the overall magnetic topology, the ambient plasma parameters, and the duration of the unstable driver. This article is part of the theme issue ‘Solar eruptions and their space weather impact’.

APA, Harvard, Vancouver, ISO, and other styles

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

Full text

Abstract:

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 in situ with particle detectors on spacecraft. In particular, particle spectra can be diagnostic of flare acceleration processes. On the other hand, energetic processes on the sun can be studied indirectly, via observations of the electromagnetic emissions (radio, X-ray, gamma-ray) produced by the particles in their interactions with the solar atmosphere. The purpose of this article is to give a brief overview on current models on particle acceleration and the present status of observations of solar energetic particles.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 of 26Al (half-life ≈0.7 megayears) in lunar samples from the Apollo mission, and present the first direct reconstruction (i.e., without any a priori assumptions) of the mean energy spectrum of solar and galactic energetic particles over a million of years. Results. We show that the reconstructed spectrum of solar energetic particles is totally consistent with that over the last decades, despite the very different levels of solar modulation of galactic cosmic rays (ϕ = 496 ± 40 MV over a million years versus (ϕ = 660 ± 20 MV for the modern epoch). We also estimated the occurrence probability of extreme solar events and argue that no events with the F(>30 MeV) fluence exceeding 5×1010 and 1011 cm−2 are expected on timescales of a thousand and million years, respectively. Conclusions. We conclude that the mean flux of solar energetic particles hardly depends on the level of solar activity, in contrast to the solar modulation of galactic cosmic rays. This puts new observational constraints on solar physics and becomes important for assessing radiation hazards for the planned space missions.

APA, Harvard, Vancouver, ISO, and other styles

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

Full text

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 unexplored region. To enable the global research community to efficiently use IS⊙IS data, we have developed an online living catalog of energetic particle enhancements observed by the IS⊙IS instruments. Event identification methodology, information on accessing the catalog, highlights of several events, and a summary of the overall trends are presented. Also included is a summary Event Catalog showing many of the key event parameters for IS⊙IS events to the time of writing.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 Advanced Composition Explorer, ACE) using a corotation time delay estimation, and energetic proton spectra from each spacecraft are compared. We find that (1) energetic protons are observed near 46 R s streaming sunward ahead of the CIR; (2) the CIR persists for at least one solar rotation and the corresponding energetic proton enhancements are observed at STEREO-A, SolO, and ACE; and (3) the proton energy spectrum is steeper near the Sun and hardens near 1 au. This observation presents the closest in situ energetic particle observation of a CIR to the Sun ever recorded. Results presented here suggest that particles can be accelerated by CIR structures within 1 au and these particles can penetrate very deep into the inner heliosphere.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 (mass, charge, energy, and propagation direction) on the particle transport, the particle energy changes in the transport process, and the effects the energetic particles have on the solar-wind plasma. The evolution of the distribution function of the energetic particles can be measured with ERNE to a better accuracy than ever before. This gives us the opportunity to contribute significantly to the modeling of interplanetary transport and acceleration. Once the acceleration/transport bias has been removed, the acceleration-site abundance of elements and their isotopes can be studied in detail and compared with spectroscopic observations.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 event shows a rough agreement with the particle density as a function of time and good agreement with the spectrum of maximum intensity values.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 R ⊙ (∼0.19 au). The CME interaction is accompanied by an intense interplanetary type II radio enhancement. Such direct measurement of particle acceleration during interplanetary CME interaction/radio enhancement is rarely recorded in previous studies. The third stage of energetic storm particles is associated with the CME-driven shock passage of the PSP at ∼0.38 au. Obviously, harder particle spectra are found in the latter two stages than the first one, which can arise from a stronger shock produced by the CME interaction and the enriched seed particles inside the preceding CME.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 omnidirectional energetic particle intensities from the observations of Energetic and Relativistic Nuclei and Electrons (ERNE), which is an energetic particle detector onboard the three-axis stabilized SOHO spacecraft. The omnidirectional intensities are calculated by fitting an exponential pitch angle distribution from directional information of energetic protons observed by ERNE. The results of the analysis show that, compared to a much faster and more intensive CMEs observed during the previous solar maximum, the acceleration efficiency decreases fast when the shock propagates outward from the Sun. The particles injected at distances <0.5 AU from the Sun dominate the particle flux during the whole period, when the shock propagates to the site of the spacecraft. The main portion of particles injected by the shock during its propagation further outward from the Sun are trapped around the shock, and are seen as an intensity increase at the time of the shock passage.Key words: Interplanetary physics (interplanetary shocks) – Solar physics, astrophysics and astronomy (energetic particles; flares and mass ejections)

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 particle energization in the supersonic solar wind via numerous dynamically interacting SMIs. AEPEs possess energies that overlap SEP events and can be an important component in understanding space weather.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

APA, Harvard, Vancouver, ISO, and other styles

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

Full text

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

APA, Harvard, Vancouver, ISO, and other styles

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

Full text

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 individual solar cycles and also from cycle to cycle. Particle propagation is controlled by spatially and temporally varying interplanetary magnetic fields, frozen into the solar wind. An overview is presented of the main heliospheric components and processes, and also of the relevant missions and data sets. Particular attention is given to flux variations over the last few solar cycles, and to extrapolated effects on the terrestrial environment.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 are modulated by the heliospheric magnetic field. In my contribution, both the current knowledge and hypotheses about modulation and the transport of cosmic rays in the heliosphere are reviewed.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 energetic electron intensities which can be accounted for by either a detached or an attached magnetic field topology for the ICME; (B) during the traversal of the out-of-ecliptic ICME event observed in July 2000 energetic electrons injected at the Sun are channeled by the ICME and propagate freely along the ICME magnetic field lines to 62° S heliolatitude.Key words. Interplanetary physics (energetic particles; interplanetary magnetic fields)

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 focused transport equation (FTE) in a stochastic manner. Particles are propagated in a solar wind generated by the newly developed data-driven heliospheric model, EUHFORIA. In this work, we solve the FTE, including all solar wind effects, cross-field diffusion, and magnetic-field gradient and curvature drifts. As initial conditions, we assume a delta injection of 4 MeV protons, spread uniformly over a selected region at the inner boundary of the model. To verify the model, we first propagate particles in nominal undisturbed fast and slow solar winds. Thereafter, we simulate and analyse the propagation of particles in a solar wind containing a corotating interaction region (CIR). We study the particle intensities and anisotropies measured by a fleet of virtual observers located at different positions in the heliosphere, as well as the global distribution of particles in interplanetary space. Results. The differential intensity-time profiles obtained in the simulations using the nominal Parker solar wind solutions illustrate the considerable adiabatic deceleration undergone by SEPs, especially when propagating in a fast solar wind. In the case of the solar wind containing a CIR, we observe that particles adiabatically accelerate when propagating in the compression waves bounding the CIR at small radial distances. In addition, for r ≳ 1.5 AU, there are particles accelerated by the reverse shock as indicated by, for example, the anisotropies and pitch-angle distributions of the particles. Moreover, a decrease in high-energy particles at the stream interface (SI) inside the CIR is observed. The compression/shock waves and the magnetic configuration near the SI may also act as a magnetic mirror, producing long-lasting high intensities at small radial distances. We also illustrate how the efficiency of the cross-field diffusion in spreading particles in the heliosphere is enhanced due to compressed magnetic fields. Finally, the inclusion of cross-field diffusion enables some particles to cross both the forward compression wave at small radial distances and the forward shock at larger radial distances. This results in the formation of an accelerated particle population centred on the forward shock, despite the lack of magnetic connection between the particle injection region and this shock wave. Particles injected in the fast solar wind stream cannot reach the forward shock since the SI acts as a diffusion barrier.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 conditions in the Earth’s environment corresponding to solar proton event. It was shown that during the early phase of the event energetic particle penetration into the magnetosphere took place in the regions on the magnetopause where the magnetospheric and interplanetary magnetic field vectors are parallel. Complex analysis of the experimental data on particle fluxes in the interplanetary medium (data from ACE spacecraft) and on low-altitude (POES) and geosynchronous (GOES) orbits inside the Earth’s magnetosphere show two regions on the magnetopause responsible for particle access to the magnetosphere: the near equatorial day-side region and open field lines window at the high-latitude magnetospheric boundary. Calculations in terms of A2000 magnetospheric magnetic field model and comparison with SuperDARN images support the link between high-latitude solar energetic particle precipitations and the region at the magnetopause where the magnetospheric field is coupled with northward IMF, allowing solar particles entrance into the magnetosphere and access to the northern polar cap.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 solar wind during the event and the coronal mass ejection (CME) that generated it. We then combine these results with the energetic particle transport model PARADISE (PArticle Radiation Asset Directed at Interplanetary Space Exploration). We find that the structure of the CME-driven shock was affected by the nonuniform solar wind, especially near the HSS, resulting in a shock wave front with strong variations in its properties such as its compression ratio and obliquity. By scaling the emission of energetic particles from the shock to the solar wind compression at the shock, an excellent match between the PARADISE simulation and in situ measurements of ≲5 MeV ions is obtained. Our modeling shows that the intricate intensity variations observed at both ACE and Bepi were influenced by the nonuniform emission of energetic particles from the deformed shock wave and demonstrates the influence of even modest background solar wind structures on the development of SEP events.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 later stages of the mission. The EPD will measure electrons, protons, and heavy ions with high temporal resolution over a wide energy range, from suprathermal energies up to several hundreds of megaelectronvolts/nucleons. For this purpose, EPD is composed of four units: the SupraThermal Electrons and Protons (STEP), the Electron Proton Telescope (EPT), the Suprathermal Ion Spectrograph (SIS), and the High-Energy Telescope (HET) plus the Instrument Control Unit that serves as power and data interface with the spacecraft. The low-energy population of electrons and ions will be covered by STEP and EPT, while the high-energy range will be measured by HET. Elemental and isotopic ion composition measurements will be performed by SIS and HET, allowing full particle identification from a few kiloelectronvolts up to several hundreds of megaelectronvolts/nucleons. Angular information will be provided by the separate look directions from different sensor heads, on the ecliptic plane along the Parker spiral magnetic field both forward and backwards, and out of the ecliptic plane observing both northern and southern hemispheres. The unparalleled observations of EPD will provide key insights into long-open and crucial questions about the processes that govern energetic particles in the inner heliosphere.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 Hurst exponent. We compare the Hurst exponent of SEP proton fluxes having energies (>1MeV to >100 MeV) for different periods, which include both solar maximum and minimum years, in order to find whether SC-dependent self-similarity exist for SEP flux.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 information about the relative contribution of the various particle sources and the major acceleration processes to the energetic particle populations. Emphasis will be put on recent studies of the source populations and the acceleration processes in the Earth’s auroral zones and magnetotail. Furthermore, the Jovian system with the largest magnetosphere and its unique mixture of particle sources with strong contributions from moons will be highlighted in some results fromUlysses.Subject headings:acceleration of particles — planets and satellites: general

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 expansion respectively, both working simultaneously in class II events, which are the most favorable to the ejection of energetic particles out of flaring sites.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 with the observations of the corresponding solar flares, radio bursts, and in situ magnetic fields and particles, we try to analyze the series of solar eruptions during October 28–November 2 as well as their correspondences with the in situ features. It is found that the difference in SEP features between the two CMEs is mainly due to (1) the seed particles probably supplied by associated flares and (2) the magnetic connection influenced by the preceding solar wind speed.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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-driven shock with an upstream component. We show the effect of varying parameters of the shock acceleration model, specifically α, the exponent of the power law in momentum of the mean free path, and η, a measure of the relative turbulence level. The main result is that including the upstream component significantly increases the flux at 1 au for typically assumed parameters in the energy range of the STEREO observation. We also derive the form of the ENA transport equation that we used in this study. These results enable a better understanding of potential observations of ENAs due to SEPs.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 Ulysses are 1.06 to 2.45 times the length of a Parker spiral magnetic field line connecting the spacecraft to the Sun. The time of particle release from the Sun is between 100 and 350 min later than the release time derived from in-ecliptic measurements. We find no evidence of correlation between the delay in release and the inverse of the speed of the CME associated with the event, or the inverse of the speed of the corresponding interplanetary shock. The main parameter determining the magnitude of the delay appears to be the difference in latitude between the flare and the footpoint of the spacecraft.Key words. Interplanetary physics (energetic particles) – Solar physics, astrophysics and astronomy (energetic particles, flares and mass ejections)

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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, with the magnetic field and solar wind velocity field from MHD results. For comparison, the 3D EPT model results with Parker fields are also obtained. We investigate the transport of SEPs with particle sources and observers in different positions in MHD fields with a CIR, and we compare the results with those in the Parker fields. Our simulation results show that the compression region with local enhancement of the magnetic field, i.e., CIR, can act as a barrier to scatter energetic particles back, and particles can struggle to diffuse through the strong magnetic field regions. Usually, a normal anisotropy profile is commonly present in SEP simulation results with Parker fields, and it is also typically present in that with MHD fields. However, because of the compression region of the magnetic field, energetic particles may exhibit anomalous anisotropy. This result may be used to replicate the spacecraft observation phenomena of the anomalous anisotropy.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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 agency (NASA) in collaboration with the European Space Agency (ESA). The satellite research (GOES) to observe the solar X-rays flare, as well as satellite research (WIND WAVE) which has been used to detect solar radiation emissions, in addition to the data we have obtained from the International Space Station (SOHO) . The study was conducted for a full year (2012) at the maximum active of the solar cycle (24), where the analysis of all the data that have been obtained. The main objective of the research is to investigate the direct link between the solar soft X-ray and non- thermal solar particles reaching the ground. The study found that the soft X-rays class X resulting from solar flare be associated with solar particle stimulant SEPs generated and to the fact that radiation generated by a class X is composed at the same time in which it occurs explosions of coronal mass ejections CMEs.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

Abstract:

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.

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

APA, Harvard, Vancouver, ISO, and other styles

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.

Full text

APA, Harvard, Vancouver, ISO, and other styles

We offer discounts on all premium plans for authors whose works are included in thematic literature selections. Contact us to get a unique promo code!