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Zhang LQ, Wang C, Baumjohann W, Wang RS, Wang JY, Burch JL, Khotyaintsev YV. First observation of fluid-like eddy-dominant bursty bulk flow turbulence in the Earth's tail plasma sheet. Sci Rep 2023; 13:19201. [PMID: 37932297 PMCID: PMC10628178 DOI: 10.1038/s41598-023-45867-w] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/19/2023] [Accepted: 10/25/2023] [Indexed: 11/08/2023] Open
Abstract
Turbulence is a ubiquitous phenomenon in neutral and conductive fluids. According to classical theory, turbulence is a rotating flow containing vortices of different scales. Eddies play a fundamental role in the nonlinear cascade of kinetic energy at different scales in turbulent flow. In conductive fluids, the Alfvénic/kinetic Alfvénic wave (AW/KAW) is the new "cell" of magnetohydrodynamic (MHD) turbulence (frozen-in condition). Wave energy, which has equal kinetic and magnetic energy, is redistributed among multiple-scale Fourier modes and transferred from the large MHD scale to the small kinetic scale through the collision of counter-propagating Alfvénic wave packages propagating along the magnetic field line. Fluid-like eddy-dominant plasma flow turbulence has never been found in space since the launch of the first satellite in 1957. In this paper, we report the first observation of eddy-dominant turbulence within magnetic reconnection-generated fast flow in the Earth's tail plasma sheet by the Magnetospheric Multiscale Spacecraft (MMS). In eddy-dominant turbulent reconnection jet, ions dominate the flow field while electrons dominate current and magnetic fluctuations. Our findings shed new light on the nonlinear kinetic and magnetic energy cascade in MHD turbulence.
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Affiliation(s)
- L Q Zhang
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing, 100080, China
| | - Chi Wang
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing, 100080, China.
| | - W Baumjohann
- Space Research Institute, Austrian Academy of Sciences, 8042, Graz, Austria
| | - R S Wang
- CAS KCAS Key Laboratory of Geospace Environment, Department of Geophysics and Planetary Science, University of Science and Technology of China, Hefei, 230026, China
| | - J Y Wang
- Information Engineering College, Central University for Nationalities, Beijing, 100081, China
| | - James L Burch
- Southwest Research Institute San Antonio, San Antonio, TX, 78238, USA
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Hashemzadeh M. Discrete eigenmodes of filamentation instability in the presence of a q-nonextensive distribution. Phys Rev E 2020; 101:013202. [PMID: 32069659 DOI: 10.1103/physreve.101.013202] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/17/2018] [Indexed: 11/07/2022]
Abstract
Discrete eigenmodes of the filamentation instability in a weakly ionized current-driven plasma in the presence of a q-nonextensive electron velocity distribution is investigated. Considering the kinetic theory, Bhatnagar-Gross-Krook collision model, and Lorentz transformation relations, the generalized longitudinal and transverse dielectric permittivities are obtained. Taking into account the long-wavelength limit and diffusion frequency limit, the dispersion relations are obtained. Using the approximation of geometrical optics and linear inhomogeneity of the plasma, the real and imaginary parts of the frequency are discussed in these limits. It is shown that in the long-wavelength limit, when the normalized electron velocity is increased the growth rate of the instability increases. However, when the collision frequency is increased the growth rate of the filamentation instability decreases. In the diffusion frequency limit, results indicate that the effects of the electron velocity and q-nonextensive parameter on the growth rate of the instability are similar. Finally, it is found that when the collision frequency is increased the growth rate of the instability increases in the presence of a q-nonextensive distribution.
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Affiliation(s)
- M Hashemzadeh
- Faculty of Physics, Shahrood University of Technology, Shahrood, Semnan Province, Iran
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Fletcher LN, de Pater I, Orton GS, Hofstadter MD, Irwin PGJ, Roman MT, Toledo D. Ice Giant Circulation Patterns: Implications for Atmospheric Probes. SPACE SCIENCE REVIEWS 2020. [PMID: 32165773 DOI: 10.1007/s11214-019-0619-5] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/04/2023]
Abstract
Atmospheric circulation patterns derived from multi-spectral remote sensing can serve as a guide for choosing a suitable entry location for a future in situ probe mission to the Ice Giants. Since the Voyager-2 flybys in the 1980s, three decades of observations from ground- and space-based observatories have generated a picture of Ice Giant circulation that is complex, perplexing, and altogether unlike that seen on the Gas Giants. This review seeks to reconcile the various competing circulation patterns from an observational perspective, accounting for spatially-resolved measurements of: zonal albedo contrasts and banded appearances; cloud-tracked zonal winds; temperature and para-H2 measurements above the condensate clouds; and equator-to-pole contrasts in condensable volatiles (methane, ammonia, and hydrogen sulphide) in the deeper troposphere. These observations identify three distinct latitude domains: an equatorial domain of deep upwelling and upper-tropospheric subsidence, potentially bounded by peaks in the retrograde zonal jet and analogous to Jovian cyclonic belts; a mid-latitude transitional domain of upper-tropospheric upwelling, vigorous cloud activity, analogous to Jovian anticyclonic zones; and a polar domain of strong subsidence, volatile depletion, and small-scale (and potentially seasonally-variable) convective activity. Taken together, the multi-wavelength observations suggest a tiered structure of stacked circulation cells (at least two in the troposphere and one in the stratosphere), potentially separated in the vertical by (i) strong molecular weight gradients associated with cloud condensation, and by (ii) transitions from a thermally-direct circulation regime at depth to a wave- and radiative-driven circulation regime at high altitude. The inferred circulation can be tested in the coming decade by 3D numerical simulations of the atmosphere, and by observations from future world-class facilities. The carrier spacecraft for any probe entry mission must ultimately carry a suite of remote-sensing instruments capable of fully constraining the atmospheric motions at the probe descent location.
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Affiliation(s)
- Leigh N Fletcher
- 1School of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH UK
| | - Imke de Pater
- 3Department of Astronomy, University of California, 501 Campbell Hall, Berkeley, CA 94720 USA
| | - Glenn S Orton
- 2Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109 USA
| | - Mark D Hofstadter
- 2Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109 USA
| | - Patrick G J Irwin
- 4Atmospheric, Oceanic and Planetary Physics, University of Oxford, Parks Road, Oxford, OX1 3PU UK
| | - Michael T Roman
- 1School of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH UK
| | - Daniel Toledo
- 4Atmospheric, Oceanic and Planetary Physics, University of Oxford, Parks Road, Oxford, OX1 3PU UK
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Antonova EE, Vorobjev VG, Kirpichev IP, Yagodkina OI, Stepanova MV. Problems with mapping the auroral oval and magnetospheric substorms. EARTH, PLANETS, AND SPACE : EPS 2015; 67:166. [PMID: 27656099 PMCID: PMC5012350 DOI: 10.1186/s40623-015-0336-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 04/30/2015] [Accepted: 10/01/2015] [Indexed: 06/06/2023]
Abstract
Accurate mapping of the auroral oval into the equatorial plane is critical for the analysis of aurora and substorm dynamics. Comparison of ion pressure values measured at low altitudes by Defense Meteorological Satellite Program (DMSP) satellites during their crossings of the auroral oval, with plasma pressure values obtained at the equatorial plane from Time History of Events and Macroscale Interactions during Substorms (THEMIS) satellite measurements, indicates that the main part of the auroral oval maps into the equatorial plane at distances between 6 and 12 Earth radii. On the nightside, this region is generally considered to be a part of the plasma sheet. However, our studies suggest that this region could form part of the plasma ring surrounding the Earth. We discuss the possibility of using the results found here to explain the ring-like shape of the auroral oval, the location of the injection boundary inside the magnetosphere near the geostationary orbit, presence of quiet auroral arcs in the auroral oval despite the constantly high level of turbulence observed in the plasma sheet, and some features of the onset of substorm expansion.
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Affiliation(s)
- E. E. Antonova
- Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow, Russia
| | - V. G. Vorobjev
- Polar Geophysical Institute, Apatity, Murmansk Region Russia
| | | | - O. I. Yagodkina
- Polar Geophysical Institute, Apatity, Murmansk Region Russia
| | - M. V. Stepanova
- Physics Department, Science Faculty, Universidad de Santiago de Chile, Santiago, Chile
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Borovsky JE, Cayton TE. Entropy mapping of the outer electron radiation belt between the magnetotail and geosynchronous orbit. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2011ja016470] [Citation(s) in RCA: 31] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Joseph E. Borovsky
- Los Alamos National Laboratory; Los Alamos New Mexico USA
- Department of Atmospheric Oceanic and Space Science; University of Michigan; Ann Arbor Michigan USA
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Materassi M, Consolini G. Magnetic reconnection rate in space plasmas: a fractal approach. PHYSICAL REVIEW LETTERS 2007; 99:175002. [PMID: 17995340 DOI: 10.1103/physrevlett.99.175002] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/13/2007] [Indexed: 05/25/2023]
Abstract
Magnetic reconnection is generally discussed via a fluid description. Here, we evaluate the reconnection rate assuming a fractal topology of the reconnection region. The central idea is that the fluid hypothesis may be violated at the scales where reconnection takes place. The reconnection rate, expressed as the Alfvén Mach number of the plasma moving toward the diffusion region, is shown to depend on the fractal dimension and on the sizes of the reconnection or diffusion region. This mechanism is more efficient than prediction of the Sweet-Parker model and even Petschek's model for finite magnetic Reynolds number. A good agreement also with rates given by Hall MHD models is found. A discussion of the fractal assumption on the diffusion region in terms of current microstructures is proposed. The comparison with in-situ satellite observations suggests the reconnection region to be a filamentary domain.
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Affiliation(s)
- Massimo Materassi
- Istituto dei Sistemi Complessi, Consiglio Nazionale delle Ricerche, V. Madonna del Piano 10, I-50019 Sesto Fiorentino, Italy. massimo.materassi@fi..isc.cnr.it
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Weygand JM, Matthaeus WH, Dasso S, Kivelson MG, Walker RJ. Taylor scale and effective magnetic Reynolds number determination from plasma sheet and solar wind magnetic field fluctuations. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2007ja012486] [Citation(s) in RCA: 38] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- James M. Weygand
- Institute of Geophysics and Planetary Physics; University of California; Los Angeles California USA
| | - W. H. Matthaeus
- Bartol Research Institute and Department of Physics and Astronomy; University of Delaware; Delaware USA
| | - S. Dasso
- Instituto de Astronomía y Física del Espacio (IAFE) and Departmento de Física, Facultad de Ciencias Exactas y Naturales; Universidad de Buenos Aires; Argentina
| | - M. G. Kivelson
- Institute of Geophysics and Planetary Physics; University of California; Los Angeles California USA
| | - R. J. Walker
- Institute of Geophysics and Planetary Physics; University of California; Los Angeles California USA
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