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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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Borrini G, Gosling JT, Bame SJ, Feldman WC, Wilcox JM. Solar wind helium and hydrogen structure near the heliospheric current sheet: A signal of coronal streamers at 1 AU. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/ja086ia06p04565] [Citation(s) in RCA: 235] [Impact Index Per Article: 19.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Richardson IG, Barbier LM, Reames DV, von Rosenvinge TT. Corotating MeV/amu ion enhancements at ≤1 AU from 1978 to 1986. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/92ja01837] [Citation(s) in RCA: 103] [Impact Index Per Article: 8.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Gosling JT, Hildner E, Asbridge JR, Bame SJ, Feldman WC. Noncompressive density enhancements in the solar wind. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/ja082i032p05005] [Citation(s) in RCA: 83] [Impact Index Per Article: 6.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Went DR, Hospodarsky GB, Masters A, Hansen KC, Dougherty MK. A new semiempirical model of Saturn's bow shock based on propagated solar wind parameters. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010ja016349] [Citation(s) in RCA: 33] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- D. R. Went
- Blackett Laboratory; Imperial College London; London UK
| | - G. B. Hospodarsky
- Department of Physics and Astronomy; University of Iowa; Iowa City Iowa USA
| | - A. Masters
- Centre for Planetary Sciences; University College London/Birkbeck; London UK
- Mullard Space Science Laboratory, Department of Space and Climate Physics; University College London; Dorking UK
| | - K. C. Hansen
- Space Research Building; University of Michigan; Ann Arbor Michigan USA
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Hollweg JV. Generation of the fast solar wind: A review with emphasis on the resonant cyclotron interaction. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2001ja000270] [Citation(s) in RCA: 272] [Impact Index Per Article: 12.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Wang YM, Sheeley NR, Socker DG, Howard RA, Rich NB. The dynamical nature of coronal streamers. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/2000ja000149] [Citation(s) in RCA: 165] [Impact Index Per Article: 6.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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McComas DJ, Barraclough BL, Funsten HO, Gosling JT, Santiago-Muñoz E, Skoug RM, Goldstein BE, Neugebauer M, Riley P, Balogh A. Solar wind observations over Ulysses' first full polar orbit. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999ja000383] [Citation(s) in RCA: 363] [Impact Index Per Article: 15.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Wimmer-Schweingruber RF, von Steiger R, Paerli R. Solar wind stream interfaces in corotating interaction regions: SWICS/Ulysses results. ACTA ACUST UNITED AC 1997. [DOI: 10.1029/97ja00951] [Citation(s) in RCA: 72] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Abstract
There are two states of the solar wind: quasi-stationary and transient. After 30 years of measurements by interplanetary spacecraft, the differences in the physical properties of the two types of wind are fairly well determined, but the physical processes involved in their accelerations are not yet understood in detail. The solar wind exists in part because the upper solar atmosphere, called the corona, is very hot, but the heating mechanisms are also not well understood. Recent research suggests a link between the heating and acceleration mechanisms.
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Neugebauer M, Alexander CJ. Shuffling foot points and magnetohydrodynamic discontinuities in the solar wind. ACTA ACUST UNITED AC 1991. [DOI: 10.1029/91ja00566] [Citation(s) in RCA: 28] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Pilipp WG, Miggenrieder H, Mühläuser KH, Rosenbauer H, Schwenn R. Large-scale variations of thermal electron parameters in the solar wind between 0.3 and 1 AU. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/ja095ia05p06305] [Citation(s) in RCA: 101] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Vellante M, Lazarus AJ. An analysis of solar wind fluctuations between 1 and 10 AU. ACTA ACUST UNITED AC 1987. [DOI: 10.1029/ja092ia09p09893] [Citation(s) in RCA: 64] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Galvin AB, Ipavich FM, Gloeckler G, Hovestadt D, Bame SJ, Klecker B, Scholer M, Tsurutani BT. Solar wind iron charge states preceding a driver plasma. ACTA ACUST UNITED AC 1987. [DOI: 10.1029/ja092ia11p12069] [Citation(s) in RCA: 38] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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van Nes P, Reinhard R, Sanderson TR, Wenzel KP, Zwickl RD. The energy spectrum of 35- to 1600-keV protons associated with interplanetary shocks. ACTA ACUST UNITED AC 1984. [DOI: 10.1029/ja089ia04p02122] [Citation(s) in RCA: 125] [Impact Index Per Article: 3.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Borrini G, Gosling JT, Bame SJ, Feldman WC. An analysis of shock wave disturbances observed at 1 AU from 1971 through 1978. ACTA ACUST UNITED AC 1982. [DOI: 10.1029/ja087ia06p04365] [Citation(s) in RCA: 110] [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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Gosling JT, Borrini G, Asbridge JR, Bame SJ, Feldman WC, Hansen RT. Coronal streamers in the solar wind at 1 AU. ACTA ACUST UNITED AC 1981. [DOI: 10.1029/ja086ia07p05438] [Citation(s) in RCA: 228] [Impact Index Per Article: 5.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Thomas BT, Smith EJ. The Parker spiral configuration of the interplanetary magnetic field between 1 and 8.5 AU. ACTA ACUST UNITED AC 1980. [DOI: 10.1029/ja085ia12p06861] [Citation(s) in RCA: 80] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Scholer M, Morfill G, Van Hollebeke MAI. On the origin of corotating energetic particle events. ACTA ACUST UNITED AC 1980. [DOI: 10.1029/ja085ia04p01743] [Citation(s) in RCA: 22] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Pizzo VJ. A three-dimensional model of corotating streams in the solar wind 2. Hydrodynamic streams. ACTA ACUST UNITED AC 1980. [DOI: 10.1029/ja085ia02p00727] [Citation(s) in RCA: 47] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Bame S, Asbridge J, Feldman W, Gosling J, Paschmann G, Sckopke N. Deceleration of the solar wind upstream from the Earth's bow shock and the origin of diffuse upstream ions. ACTA ACUST UNITED AC 1980. [DOI: 10.1029/ja085ia06p02981] [Citation(s) in RCA: 111] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Krimigis SM, Armstrong TP, Axford WI, Bostrom CO, Fan CY, Gloeckler G, Lanzerotti LJ, Keath EP, Zwickl RD, Carbary JF, Hamilton DC. Low-Energy Charged Particle Environment at Jupiter: A First Look. Science 1979; 204:998-1003. [PMID: 17800439 DOI: 10.1126/science.204.4396.998] [Citation(s) in RCA: 123] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The low-energy charged particle instrument on Voyager was designed to measure the hot plasma (electron and ion energies greater, similar 15 and greater, similar 30 kiloelectron volts, respectively) component of the Jovian magnetosphere. Protons, heavier ions, and electrons at these energies were detected nearly a third of an astronomical unit before encounter with the planet. The hot plasma near the magnetosphere boundary is predominantly composed of protons, oxygen, and sulfur in comparable proportions and a nonthermal power-law tail; its temperature is about 3 x 10(8) K, density about 5 x 10(-3) per cubic centimeter, and energy density comparable to that of the magnetic field. The plasma appears to be corotating throughout the magnetosphere; no hot plasma outflow, as suggested by planetary wind theories, is observed. The main constituents of the energetic particle population ( greater, similar200 kiloelectron volts per nucleon) are protons, helium, oxygen, sulfur, and some sodium observed throughout the outer magnetosphere; it is probable that the sulfur, sodium, and possibly oxygen originate at 1o. Fluxes in the outbound trajectory appear to be enhancedfrom approximately 90 degrees to approximately 130 degrees longitude (System III). Consistent low-energy particle flux periodicities were not observed on the inbound trajectory; both 5-and 10-hour periodicities were observed on the outbound trajectory. Partial absorption of > 10 million electron volts electrons is observed in the vicinity of the Io flux tube.
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Feldman WC, Asbridge JR, Bame SJ, Gosling JT. Long-term variations of selected solar wind properties: Imp 6, 7, and 8 results. ACTA ACUST UNITED AC 1978. [DOI: 10.1029/ja083ia05p02177] [Citation(s) in RCA: 131] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Joselyn J, Holzer TE. A steady three-fluid coronal expansion for nonspherical geometries. ACTA ACUST UNITED AC 1978. [DOI: 10.1029/ja083ia03p01019] [Citation(s) in RCA: 50] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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