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Element Abundances of Solar Energetic Particles and the Photosphere, the Corona, and the Solar Wind. ATOMS 2019. [DOI: 10.3390/atoms7040104] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/16/2022] Open
Abstract
From a turbulent history, the study of the abundances of elements in solar energetic particles (SEPs) has grown into an extensive field that probes the solar corona and physical processes of SEP acceleration and transport. Underlying SEPs are the abundances of the solar corona, which differ from photospheric abundances as a function of the first ionization potentials (FIPs) of the elements. The FIP-dependence of SEPs also differs from that of the solar wind; each has a different magnetic environment, where low-FIP ions and high-FIP neutral atoms rise toward the corona. Two major sources generate SEPs: The small “impulsive” SEP events are associated with magnetic reconnection in solar jets that produce 1000-fold enhancements from H to Pb as a function of mass-to-charge ratio A/Q, and also 1000-fold enhancements in 3He/4He that are produced by resonant wave-particle interactions. In large “gradual” events, SEPs are accelerated at shock waves that are driven out from the Sun by wide, fast coronal mass ejections (CMEs). A/Q dependence of ion transport allows us to estimate Q and hence the source plasma temperature T. Weaker shock waves favor the reacceleration of suprathermal ions accumulated from earlier impulsive SEP events, along with protons from the ambient plasma. In strong shocks, the ambient plasma dominates. Ions from impulsive sources have T ≈ 3 MK; those from ambient coronal plasma have T = 1 – 2 MK. These FIP- and A/Q-dependences explore complex new interactions in the corona and in SEP sources.
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Kilpua E, Koskinen HEJ, Pulkkinen TI. Coronal mass ejections and their sheath regions in interplanetary space. LIVING REVIEWS IN SOLAR PHYSICS 2017; 14:5. [PMID: 31997985 PMCID: PMC6956910 DOI: 10.1007/s41116-017-0009-6] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/02/2017] [Accepted: 10/03/2017] [Indexed: 06/09/2023]
Abstract
Interplanetary coronal mass ejections (ICMEs) are large-scale heliospheric transients that originate from the Sun. When an ICME is sufficiently faster than the preceding solar wind, a shock wave develops ahead of the ICME. The turbulent region between the shock and the ICME is called the sheath region. ICMEs and their sheaths and shocks are all interesting structures from the fundamental plasma physics viewpoint. They are also key drivers of space weather disturbances in the heliosphere and planetary environments. ICME-driven shock waves can accelerate charged particles to high energies. Sheaths and ICMEs drive practically all intense geospace storms at the Earth, and they can also affect dramatically the planetary radiation environments and atmospheres. This review focuses on the current understanding of observational signatures and properties of ICMEs and the associated sheath regions based on five decades of studies. In addition, we discuss modelling of ICMEs and many fundamental outstanding questions on their origin, evolution and effects, largely due to the limitations of single spacecraft observations of these macro-scale structures. We also present current understanding of space weather consequences of these large-scale solar wind structures, including effects at the other Solar System planets and exoplanets. We specially emphasize the different origin, properties and consequences of the sheaths and ICMEs.
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Affiliation(s)
- Emilia Kilpua
- Department of Physics, University of Helsinki, Helsinki, Finland
| | - Hannu E. J. Koskinen
- Department of Physics, University of Helsinki, Helsinki, Finland
- Finnish Meteorological Institute, Espoo, Finland
| | - Tuija I. Pulkkinen
- Department of Electronics and Nanoengineering, Aalto University, Espoo, Finland
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Desai M, Giacalone J. Large gradual solar energetic particle events. LIVING REVIEWS IN SOLAR PHYSICS 2016; 13:3. [PMID: 32355890 PMCID: PMC7175685 DOI: 10.1007/s41116-016-0002-5] [Citation(s) in RCA: 11] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/13/2014] [Accepted: 11/13/2015] [Indexed: 05/24/2023]
Abstract
Solar energetic particles, or SEPs, from suprathermal (few keV) up to relativistic ( ∼ few GeV) energies are accelerated near the Sun in at least two ways: (1) by magnetic reconnection-driven processes during solar flares resulting in impulsive SEPs, and (2) at fast coronal-mass-ejection-driven shock waves that produce large gradual SEP events. Large gradual SEP events are of particular interest because the accompanying high-energy ( > 10 s MeV) protons pose serious radiation threats to human explorers living and working beyond low-Earth orbit and to technological assets such as communications and scientific satellites in space. However, a complete understanding of these large SEP events has eluded us primarily because their properties, as observed in Earth orbit, are smeared due to mixing and contributions from many important physical effects. This paper provides a comprehensive review of the current state of knowledge of these important phenomena, and summarizes some of the key questions that will be addressed by two upcoming missions-NASA's Solar Probe Plus and ESA's Solar Orbiter. Both of these missions are designed to directly and repeatedly sample the near-Sun environments where interplanetary scattering and transport effects are significantly reduced, allowing us to discriminate between different acceleration sites and mechanisms and to isolate the contributions of numerous physical processes occurring during large SEP events.
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Affiliation(s)
- Mihir Desai
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238 USA
| | - Joe Giacalone
- Department of Planetary Sciences, University of Arizona, Tucson, AZ 85721 USA
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Raouafi NE, Patsourakos S, Pariat E, Young PR, Sterling A, Savcheva A, Shimojo M, Moreno-Insertis F, DeVore CR, Archontis V, Török T, Mason H, Curdt W, Meyer K, Dalmasse K, Matsui Y. Solar Coronal Jets: Observations, Theory, and Modeling. SPACE SCIENCE REVIEWS 2016; 201:1-53. [PMID: 32908324 PMCID: PMC7477949 DOI: 10.1007/s11214-016-0260-5] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/08/2023]
Abstract
Chromospheric and coronal jets represent important manifestations of ubiquitous solar transients, which may be the source of significant mass and energy input to the upper solar atmosphere and the solar wind. While the energy involved in a jet-like event is smaller than that of "nominal" solar flares and Coronal Mass Ejections (CMEs), jets share many common properties with these major phenomena, in particular, the explosive magnetically driven dynamics. Studies of jets could, therefore, provide critical insight for understanding the larger, more complex drivers of the solar activity. On the other side of the size-spectrum, the study of jets could also supply important clues on the physics of transients close or at the limit of the current spatial resolution such as spicules. Furthermore, jet phenomena may hint to basic process for heating the corona and accelerating the solar wind; consequently their study gives us the opportunity to attack a broad range of solar-heliospheric problems.
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Affiliation(s)
- N. E. Raouafi
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - S. Patsourakos
- Department of Physics, University of Ioannina, Ioannina, Greece
| | - E. Pariat
- LESIA, Observatoire de Paris, Meudon, France
| | - P. R. Young
- College of Science, George Mason University, Fairfax, VA, USA. NASA/Goddard Space Flight Center, Code 671, Greenbelt, MD 20771, USA
| | - A. Sterling
- NASA/Marshall Space Flight Center, Huntsville, Alabama, USA
| | - A. Savcheva
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA
| | - M. Shimojo
- National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
| | | | - C. R. DeVore
- Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - V. Archontis
- School of Mathematics and Statistics, University of St. Andrews, St. Andrews, UK
| | - T. Török
- Predictive Science Inc., 9990 Mesa Rim Rd., Ste. 170, San Diego, CA 92121, USA
| | - H. Mason
- DAMTP, Centre for Mathematical Sciences, University of Cambridge, Cambridge, UK
| | - W. Curdt
- Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany
| | - K. Meyer
- Division of Computing and Mathematics, Abertay University, Dundee, UK
| | - K. Dalmasse
- LESIA, Observatoire de Paris, Meudon, France
- CISL/HAO, NCAR, P.O. Box 3000, Boulder, CO 80307-3000, USA
| | - Y. Matsui
- Department of Earth and Planetary Science, University of Tokyo, Tokyo, Japan
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Energetic Particles and the Structure of Coronal Mass Ejections. ACTA ACUST UNITED AC 2013. [DOI: 10.1029/gm099p0217] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 04/30/2023]
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Forman MA, Webb GM. Acceleration of Energetic Particles. ACTA ACUST UNITED AC 2013. [DOI: 10.1029/gm034p0091] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 03/11/2023]
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Kahler SW. Coronal mass ejections and long risetimes of solar energetic particle events. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/92ja02605] [Citation(s) in RCA: 24] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Li G. Acceleration and transport of heavy ions at coronal mass ejection-driven shocks. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004ja010600] [Citation(s) in RCA: 68] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Li G, Zank GP, Rice WKM. Energetic particle acceleration and transport at coronal mass ejection-driven shocks. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2002ja009666] [Citation(s) in RCA: 130] [Impact Index Per Article: 6.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Gang Li
- Institute of Geophysics and Planetary Physics; University of California; Riverside California USA
| | - G. P. Zank
- Institute of Geophysics and Planetary Physics; University of California; Riverside California USA
| | - W. K. M. Rice
- School of Physics and Astronomy; University of St. Andrews; St. Andrews Fife UK
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Rice WKM. Particle acceleration and coronal mass ejection driven shocks: Shocks of arbitrary strength. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2002ja009756] [Citation(s) in RCA: 91] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Cane HV. Solar flares, type III radio bursts, coronal mass ejections, and energetic particles. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2001ja000320] [Citation(s) in RCA: 184] [Impact Index Per Article: 8.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Cohen CMS, Mewaldt RA, Cummings AC, Leske RA, Stone EC, Slocum PL, Wiedenbeck ME, Christian ER, von Rosenvinge TT. Forecasting the arrival of shock-accelerated solar energetic particles at Earth. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000ja000216] [Citation(s) in RCA: 14] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Turner R. Solar Particle Events from a risk management perspective. IEEE TRANSACTIONS ON PLASMA SCIENCE. IEEE NUCLEAR AND PLASMA SCIENCES SOCIETY 2000; 28:2103-2113. [PMID: 12238518 DOI: 10.1109/27.902237] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
Solar Particle Events pose a health risk to astronauts in space. Today, SPE forecasts are inadequate to provide advance warning with sufficient credibility to lead operators to initiate protective measures. However, research on SPEs and Coronal Mass Ejections suggests that the space weather community is on the verge of substantial improvements in understanding solar energetic particle acceleration and propagation. This paper describes the impact of SPEs, reviews the physics of SPEs, discusses current SPE forecast tools, and describes an approach to provide the comprehensive space weather data necessary to implement physics-based SPE risk management.
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Zank GP, Rice WKM, Wu CC. Particle acceleration and coronal mass ejection driven shocks: A theoretical model. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999ja000455] [Citation(s) in RCA: 258] [Impact Index Per Article: 10.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Reames DV, Ng CK, Tylka AJ. Initial Time Dependence of Abundances in Solar Energetic Particle Events. THE ASTROPHYSICAL JOURNAL 2000; 531:L83-L86. [PMID: 10673420 DOI: 10.1086/312517] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
We compare the initial behavior of Fe/O and He/H abundance ratios and their relationship to the evolution of the proton energy spectra in "small" and "large" gradual solar energetic particle (SEP) events. The results are qualitatively consistent with the behavior predicted by the theory of Ng et al. published in 1999. He/H ratios that initially rise with time are a signature of scattering by non-Kolmogorov Alfvén wave spectra generated by intense beams of shock-accelerated protons streaming outward in large gradual SEP events.
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Sheeley NR, Walters JH, Wang YM, Howard RA. Continuous tracking of coronal outflows: Two kinds of coronal mass ejections. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/1999ja900308] [Citation(s) in RCA: 426] [Impact Index Per Article: 17.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Abstract
In the large solar energetic particle (SEP) events that constitute a serious radiation hazard, particles are accelerated at shock waves driven out from the Sun by coronal mass ejections (CMEs). A self-regulating mechanism of wave formation by the streaming particles limits SEP intensities early in the event. Hazardous intensities do not occur until the arrival of the shock itself. This provides an opportunity to warn astronauts to take shelter after the onset of the event at the Sun and before arrival of the shock, a time of approximately 12 h or more. The actual time history of particle intensities depends strongly on the longitude of the event at the Sun, on the width the CME, and especially on the speed of the shock. Fortunately, hazardous events are relatively rare. Unfortunately, this gives us few events to study, so we are forced to extrapolate knowledge gained at lower energies in the frequent smaller events. It is essential that the spacecraft with our best instrumentation be positioned outside the Earth's magnetosphere where they can observe these rare large events when they do occur.
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Affiliation(s)
- D Reames
- NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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Kahler SW, Kunches JM, Smith DF. Role of current sheets in the modulation of solar energetic particle events. ACTA ACUST UNITED AC 1996. [DOI: 10.1029/96ja02446] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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McAllister AH, Dryer M, Mclntosh P, Singer H, Weiss L. A large polar crown coronal mass ejection and a “problem” goemagnetic storm: April 14-23, 1994. ACTA ACUST UNITED AC 1996. [DOI: 10.1029/96ja00510] [Citation(s) in RCA: 99] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Cliver EW, Feynman J, Garrett HB. An estimate of the maximum speed of the solar wind, 1938–1989. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/ja095ia10p17103] [Citation(s) in RCA: 88] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Cane HV, von Rosenvinge TT, McGuire RE. Energetic particle observations at the Helios 1 spacecraft of shocks associated with coronal mass ejections. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/ja095ia05p06575] [Citation(s) in RCA: 22] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Webb DF, Jackson BV. The identification and characteristics of solar mass ejections observed in the heliosphere by the Helios 2 photometers. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/ja095ia12p20641] [Citation(s) in RCA: 29] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Tang F, Tsurutani BT, Gonzalez WD, Akasofu SI, Smith EJ. Solar sources of interplanetary southwardBzevents responsible for major magnetic storms (1978-1979). ACTA ACUST UNITED AC 1989. [DOI: 10.1029/ja094ia04p03535] [Citation(s) in RCA: 52] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Wilson RM, Hildner E. On the association of magnetic clouds with disappearing filaments. ACTA ACUST UNITED AC 1986. [DOI: 10.1029/ja091ia05p05867] [Citation(s) in RCA: 68] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Cliver EW, McNamara LF, Gentile LC. Peak flux density spectra of large solar radio bursts and proton emission from flares. ACTA ACUST UNITED AC 1985. [DOI: 10.1029/ja090ia07p06251] [Citation(s) in RCA: 15] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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