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Zhang H, Zong Q, Connor H, Delamere P, Facskó G, Han D, Hasegawa H, Kallio E, Kis Á, Le G, Lembège B, Lin Y, Liu T, Oksavik K, Omidi N, Otto A, Ren J, Shi Q, Sibeck D, Yao S. Dayside Transient Phenomena and Their Impact on the Magnetosphere and Ionosphere. SPACE SCIENCE REVIEWS 2022; 218:40. [PMID: 35784192 PMCID: PMC9239986 DOI: 10.1007/s11214-021-00865-0] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 01/01/2021] [Accepted: 11/11/2021] [Indexed: 06/15/2023]
Abstract
Dayside transients, such as hot flow anomalies, foreshock bubbles, magnetosheath jets, flux transfer events, and surface waves, are frequently observed upstream from the bow shock, in the magnetosheath, and at the magnetopause. They play a significant role in the solar wind-magnetosphere-ionosphere coupling. Foreshock transient phenomena, associated with variations in the solar wind dynamic pressure, deform the magnetopause, and in turn generates field-aligned currents (FACs) connected to the auroral ionosphere. Solar wind dynamic pressure variations and transient phenomena at the dayside magnetopause drive magnetospheric ultra low frequency (ULF) waves, which can play an important role in the dynamics of Earth's radiation belts. These transient phenomena and their geoeffects have been investigated using coordinated in-situ spacecraft observations, spacecraft-borne imagers, ground-based observations, and numerical simulations. Cluster, THEMIS, Geotail, and MMS multi-mission observations allow us to track the motion and time evolution of transient phenomena at different spatial and temporal scales in detail, whereas ground-based experiments can observe the ionospheric projections of transient magnetopause phenomena such as waves on the magnetopause driven by hot flow anomalies or flux transfer events produced by bursty reconnection across their full longitudinal and latitudinal extent. Magnetohydrodynamics (MHD), hybrid, and particle-in-cell (PIC) simulations are powerful tools to simulate the dayside transient phenomena. This paper provides a comprehensive review of the present understanding of dayside transient phenomena at Earth and other planets, their geoeffects, and outstanding questions.
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Affiliation(s)
- Hui Zhang
- Physics Department & Geophysical Institute, University of Alaska Fairbanks, 2156 Koyukuk Drive, Fairbanks, AK 99775 USA
- Shandong University, Weihai, China
| | - Qiugang Zong
- Institute of Space Physics and Applied Technology, Peking University, Beijing, 100871 China
- Polar Research Institute of China, Shanghai, 200136 China
| | - Hyunju Connor
- Physics Department & Geophysical Institute, University of Alaska Fairbanks, 2156 Koyukuk Drive, Fairbanks, AK 99775 USA
- NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA
| | - Peter Delamere
- Physics Department & Geophysical Institute, University of Alaska Fairbanks, 2156 Koyukuk Drive, Fairbanks, AK 99775 USA
| | - Gábor Facskó
- Department of Informatics, Milton Friedman University, 1039 Budapest, Hungary
- Wigner Research Centre for Physics, Konkoly-Thege Miklós út 29-33, 1121 Budapest, Hungary
| | | | - Hiroshi Hasegawa
- Institute of Space and Astronautical Science, JAXA, Sagamihara, Japan
| | | | - Árpád Kis
- Institute of Earth Physics and Space Science (ELKH EPSS), Sopron, Hungary
| | - Guan Le
- NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA
| | - Bertrand Lembège
- LATMOS (Laboratoire Atmosphères, Milieux, Observations Spatiales), IPSL/CNRS/UVSQ, 11 Bd d’Alembert, Guyancourt, 78280 France
| | - Yu Lin
- Auburn University, Auburn, USA
| | - Terry Liu
- Physics Department & Geophysical Institute, University of Alaska Fairbanks, 2156 Koyukuk Drive, Fairbanks, AK 99775 USA
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, Los Angeles, USA
| | - Kjellmar Oksavik
- Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, Bergen, Norway
- Arctic Geophysics, The University Centre in Svalbard, Longyearbyen, Norway
| | | | - Antonius Otto
- Physics Department & Geophysical Institute, University of Alaska Fairbanks, 2156 Koyukuk Drive, Fairbanks, AK 99775 USA
| | - Jie Ren
- Institute of Space Physics and Applied Technology, Peking University, Beijing, 100871 China
| | | | - David Sibeck
- NASA Goddard Space Flight Center, Greenbelt, MD 20771 USA
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Wu SY, Ye SY, Fischer G, Jackman CM, Wang J, Menietti JD, Cecconi B, Long MY. Reflection and Refraction of the L-O Mode 5 kHz Saturn Narrowband Emission by the Magnetosheath. GEOPHYSICAL RESEARCH LETTERS 2022; 49:e2021GL096990. [PMID: 35859935 PMCID: PMC9285440 DOI: 10.1029/2021gl096990] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 11/16/2021] [Revised: 02/10/2022] [Accepted: 02/12/2022] [Indexed: 06/15/2023]
Abstract
The reflection-by-sheath mechanism of 5 kHz narrowband emissions (NB) at Saturn is confirmed by Cassini observations during several crossings of the magnetopause, which show that the 5 kHz NB can be prevented from escaping Saturn's magnetosphere. The L-O mode 5 kHz NB remained visible in areas of low plasma density but disappeared in regions of high plasma density. In three cases, NB disappeared immediately after the crossings of Saturn's magnetopause. A possible reflected NB event observed near the magnetosheath is discussed. This mechanism can help explain the 5 kHz NB observed at low latitudes outside the Enceladus plasma torus and their upper frequency limit variations. This mechanism significantly improves the current understanding of the 5 kHz NB.
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Affiliation(s)
- S. Y. Wu
- Department of Earth and Space SciencesSouthern University of Science and TechnologyShenzhenPeople's Republic of China
| | - S. Y. Ye
- Department of Earth and Space SciencesSouthern University of Science and TechnologyShenzhenPeople's Republic of China
| | - G. Fischer
- Space Research InstituteAustrian Academy of SciencesGrazAustria
| | - C. M. Jackman
- School of Cosmic PhysicsDublin Institute for Advanced StudiesDublinIreland
| | - J. Wang
- Department of Earth and Space SciencesSouthern University of Science and TechnologyShenzhenPeople's Republic of China
| | - J. D. Menietti
- Department of Physics and AstronomyUniversity of IowaIowa CityIAUSA
| | - B. Cecconi
- LESIA, Observatoire de ParisUniversité PSLCNRSSorbonne UniversitéUniversité de Paris MeudonParisFrance
| | - M. Y. Long
- Department of Space PhysicsSchool of Electronic InformationWuhan UniversityWuhanPeople's Republic of China
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Samanta T, Tian H, Nakariakov VM. Evidence for Vortex Shedding in the Sun's Hot Corona. PHYSICAL REVIEW LETTERS 2019; 123:035102. [PMID: 31386484 DOI: 10.1103/physrevlett.123.035102] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/28/2019] [Revised: 06/21/2019] [Indexed: 06/10/2023]
Abstract
Vortex shedding is an oscillating flow that is commonly observed in fluids due to the presence of a blunt body in a flowing medium. Numerical simulations have shown that the phenomenon of vortex shedding could also develop in the magnetohydrodynamic (MHD) domain. The dimensionless Strouhal number, the ratio of the blunt body diameter to the product of the period of vortex shedding and the speed of a flowing medium, is a robust indicator for vortex shedding, and, generally of the order of 0.2 for a wide range of Reynolds number. Using an observation from the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory, we report a wavelike or oscillating plasma flow propagating upward against the Sun's gravitational force. A newly formed shrinking loop in the postflare region possibly generates the oscillation of the upflow in the wake of the hot and dense loop through vortex shedding. The computed Strouhal number is consistent with the prediction from previous MHD simulations. Our observation suggests the possibility of vortex shedding in the solar corona.
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Affiliation(s)
- Tanmoy Samanta
- School of Earth and Space Sciences, Peking University, Beijing 100871, China
| | - Hui Tian
- School of Earth and Space Sciences, Peking University, Beijing 100871, China
| | - Valery M Nakariakov
- Centre for Fusion, Space and Astrophysics, University of Warwick, Coventry CV47AL, United Kingdom
- St. Petersburg Branch, Special Astrophysical Observatory, Russian Academy of Sciences, 196140 St. Petersburg, Russia
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Li X, Zhang J, Yang S, Hou Y, Erdélyi R. Observing Kelvin-Helmholtz instability in solar blowout jet. Sci Rep 2018; 8:8136. [PMID: 29802364 PMCID: PMC5970241 DOI: 10.1038/s41598-018-26581-4] [Citation(s) in RCA: 28] [Impact Index Per Article: 4.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/07/2018] [Accepted: 05/15/2018] [Indexed: 11/09/2022] Open
Abstract
Kelvin-Helmholtz instability (KHI) is a basic physical process in fluids and magnetized plasmas, with applications successfully modelling e.g. exponentially growing instabilities observed at magnetospheric and heliospheric boundaries, in the solar or Earth's atmosphere and within astrophysical jets. Here, we report the discovery of the KHI in solar blowout jets and analyse the detailed evolution by employing high-resolution data from the Interface Region Imaging Spectrograph (IRIS) satellite launched in 2013. The particular jet we focus on is rooted in the surrounding penumbra of the main negative polarity sunspot of Active Region 12365, where the main body of the jet is a super-penumbral structure. At its maximum, the jet has a length of 90 Mm, a width of 19.7 Mm, and its density is about 40 times higher than its surroundings. During the evolution of the jet, a cavity appears near the base of the jet, and bi-directional flows originated from the top and bottom of the cavity start to develop, indicating that magnetic reconnection takes place around the cavity. Two upward flows pass along the left boundary of the jet successively. Next, KHI develops due to a strong velocity shear (∼204 km s-1) between these two flows, and subsequently the smooth left boundary exhibits a sawtooth pattern, evidencing the onset of the instability.
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Affiliation(s)
- Xiaohong Li
- CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China. .,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, 100049, China.
| | - Jun Zhang
- CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China. .,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, 100049, China.
| | - Shuhong Yang
- CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China.,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, 100049, China
| | - Yijun Hou
- CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China.,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, 100049, China
| | - Robert Erdélyi
- Solar Physics and Space Plasma Research Centre, School of Mathematics and Statistics, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield, S3 7RH, UK.,Department of Astronomy, Eötvös Lorand University, Pázmány Péter sétány 1/A, Budapest, H-1117, Hungary
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Dunn WR, Branduardi-Raymont G, Elsner RF, Vogt MF, Lamy L, Ford PG, Coates AJ, Gladstone GR, Jackman CM, Nichols JD, Rae IJ, Varsani A, Kimura T, Hansen KC, Jasinski JM. The impact of an ICME on the Jovian X-ray aurora. JOURNAL OF GEOPHYSICAL RESEARCH. SPACE PHYSICS 2016; 121:2274-2307. [PMID: 27867794 PMCID: PMC5111422 DOI: 10.1002/2015ja021888] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 09/07/2015] [Revised: 01/11/2016] [Accepted: 01/27/2016] [Indexed: 06/06/2023]
Abstract
We report the first Jupiter X-ray observations planned to coincide with an interplanetary coronal mass ejection (ICME). At the predicted ICME arrival time, we observed a factor of ∼8 enhancement in Jupiter's X-ray aurora. Within 1.5 h of this enhancement, intense bursts of non-Io decametric radio emission occurred. Spatial, spectral, and temporal characteristics also varied between ICME arrival and another X-ray observation two days later. Gladstone et al. (2002) discovered the polar X-ray hot spot and found it pulsed with 45 min quasiperiodicity. During the ICME arrival, the hot spot expanded and exhibited two periods: 26 min periodicity from sulfur ions and 12 min periodicity from a mixture of carbon/sulfur and oxygen ions. After the ICME, the dominant period became 42 min. By comparing Vogt et al. (2011) Jovian mapping models with spectral analysis, we found that during ICME arrival at least two distinct ion populations, from Jupiter's dayside, produced the X-ray aurora. Auroras mapping to magnetospheric field lines between 50 and 70 RJ were dominated by emission from precipitating sulfur ions (S7+,…,14+). Emissions mapping to closed field lines between 70 and 120 RJ and to open field lines were generated by a mixture of precipitating oxygen (O7+,8+) and sulfur/carbon ions, possibly implying some solar wind precipitation. We suggest that the best explanation for the X-ray hot spot is pulsed dayside reconnection perturbing magnetospheric downward currents, as proposed by Bunce et al. (2004). The auroral enhancement has different spectral, spatial, and temporal characteristics to the hot spot. By analyzing these characteristics and coincident radio emissions, we propose that the enhancement is driven directly by the ICME through Jovian magnetosphere compression and/or a large-scale dayside reconnection event.
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Affiliation(s)
- William R Dunn
- Mullard Space Science Laboratory, Department of Space and Climate Physics University College London Dorking UK; Centre for Planetary Science UCL/Birkbeck London UK
| | | | - Ronald F Elsner
- ZP12, NASA Marshall Space Flight Center Huntsville Alabama USA
| | - Marissa F Vogt
- Center for Space Physics Boston University Boston Massachusetts USA
| | - Laurent Lamy
- LESIA, Observatoire de Paris, CNRS, UPMC Université Paris Diderot Meudon France
| | - Peter G Ford
- Kavli Institute for Astrophysics and Space Research MIT Cambridge Massachusetts USA
| | - Andrew J Coates
- Mullard Space Science Laboratory, Department of Space and Climate Physics University College London Dorking UK; Centre for Planetary Science UCL/Birkbeck London UK
| | - G Randall Gladstone
- Space Science and Engineering Division Southwest Research Institute San Antonio Texas USA
| | - Caitriona M Jackman
- Department of Physics and Astronomy University of Southampton Southampton UK
| | - Jonathan D Nichols
- Department of Physics and Astronomy University of Leicester Leicester UK
| | - I Jonathan Rae
- Mullard Space Science Laboratory, Department of Space and Climate Physics University College London Dorking UK
| | - Ali Varsani
- Mullard Space Science Laboratory, Department of Space and Climate Physics University College London Dorking UK; Space Research Institute Austrian Academy of Sciences Graz Austria
| | - Tomoki Kimura
- Institute of Space and Astronautical Science Japan Aerospace Exploration Agency Sagamihara Japan; Nishina Center for Accelerator-Based Science RIKEN Wako Japan
| | - Kenneth C Hansen
- Department of Atmospheric, Oceanic and Space Sciences University of Michigan Ann Arbor Michigan USA
| | - Jamie M Jasinski
- Mullard Space Science Laboratory, Department of Space and Climate Physics University College London Dorking UK; Centre for Planetary Science UCL/Birkbeck London UK; Department of Atmospheric, Oceanic and Space Sciences University of Michigan Ann Arbor Michigan USA
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Desroche M, Bagenal F, Delamere PA, Erkaev N. Conditions at the expanded Jovian magnetopause and implications for the solar wind interaction. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2012ja017621] [Citation(s) in RCA: 43] [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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Jia X, Kivelson MG, Gombosi TI. Driving Saturn's magnetospheric periodicities from the upper atmosphere/ionosphere. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011ja017367] [Citation(s) in RCA: 48] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Wilson RJ, Delamere PA, Bagenal F, Masters A. Kelvin-Helmholtz instability at Saturn's magnetopause: Cassini ion data analysis. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011ja016723] [Citation(s) in RCA: 35] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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9
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Badman SV, Achilleos N, Arridge CS, Baines KH, Brown RH, Bunce EJ, Coates AJ, Cowley SWH, Dougherty MK, Fujimoto M, Hospodarsky G, Kasahara S, Kimura T, Melin H, Mitchell DG, Stallard T, Tao C. Cassini observations of ion and electron beams at Saturn and their relationship to infrared auroral arcs. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011ja017222] [Citation(s) in RCA: 44] [Impact Index Per Article: 3.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Delamere PA, Wilson RJ, Masters A. Kelvin-Helmholtz instability at Saturn's magnetopause: Hybrid simulations. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2011ja016724] [Citation(s) in RCA: 53] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- P. A. Delamere
- Laboratory for Atmospheric and Space Physics; University of Colorado; Boulder Colorado USA
| | - R. J. Wilson
- Laboratory for Atmospheric and Space Physics; University of Colorado; Boulder Colorado USA
| | - A. Masters
- Mullard Space Science Laboratory, Department of Space and Climate Physics; University College London; Holmbury St. Mary UK
- Centre for Planetary Sciences at UCL/Birkbeck; London UK
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Grodent D, Gustin J, Gérard JC, Radioti A, Bonfond B, Pryor WR. Small-scale structures in Saturn's ultraviolet aurora. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2011ja016818] [Citation(s) in RCA: 54] [Impact Index Per Article: 4.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- D. Grodent
- Laboratoire de Physique Atmosphérique et Planétaire; Université de Liège; Liège Belgium
| | - J. Gustin
- Laboratoire de Physique Atmosphérique et Planétaire; Université de Liège; Liège Belgium
| | - J.-C. Gérard
- Laboratoire de Physique Atmosphérique et Planétaire; Université de Liège; Liège Belgium
| | - A. Radioti
- Laboratoire de Physique Atmosphérique et Planétaire; Université de Liège; Liège Belgium
| | - B. Bonfond
- Laboratoire de Physique Atmosphérique et Planétaire; Université de Liège; Liège Belgium
| | - W. R. Pryor
- Science Department; Central Arizona College; Coolidge Arizona USA
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