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Russell DR, Burdiak GC, Carroll-Nellenback JJ, Halliday JWD, Hare JD, Merlini S, Suttle LG, Valenzuela-Villaseca V, Eardley SJ, Fullalove JA, Rowland GC, Smith RA, Frank A, Hartigan P, Velikovich AL, Chittenden JP, Lebedev SV. Perpendicular Subcritical Shock Structure in a Collisional Plasma Experiment. PHYSICAL REVIEW LETTERS 2022; 129:225001. [PMID: 36493430 DOI: 10.1103/physrevlett.129.225001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/19/2022] [Revised: 10/14/2022] [Accepted: 10/25/2022] [Indexed: 06/17/2023]
Abstract
We present a study of perpendicular subcritical shocks in a collisional laboratory plasma. Shocks are produced by placing obstacles into the supermagnetosonic outflow from an inverse wire array z pinch. We demonstrate the existence of subcritical shocks in this regime and find that secondary shocks form in the downstream. Detailed measurements of the subcritical shock structure confirm the absence of a hydrodynamic jump. We calculate the classical (Spitzer) resistive diffusion length and show that it is approximately equal to the shock width. We measure little heating across the shock (<10% of the ion kinetic energy) which is consistent with an absence of viscous dissipation.
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Affiliation(s)
- D R Russell
- Blackett Laboratory, Imperial College London, London SW7 2AZ, United Kingdom
| | - G C Burdiak
- First Light Fusion Ltd, Yarnton, Kidlington OX5 1QU, United Kingdom
| | - J J Carroll-Nellenback
- Department of Physics and Astronomy, University of Rochester, Rochester, New York 14627, USA
| | - J W D Halliday
- Blackett Laboratory, Imperial College London, London SW7 2AZ, United Kingdom
| | - J D Hare
- Plasma Science and Fusion Center, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA
| | - S Merlini
- Blackett Laboratory, Imperial College London, London SW7 2AZ, United Kingdom
| | - L G Suttle
- Blackett Laboratory, Imperial College London, London SW7 2AZ, United Kingdom
| | | | - S J Eardley
- Blackett Laboratory, Imperial College London, London SW7 2AZ, United Kingdom
| | - J A Fullalove
- Blackett Laboratory, Imperial College London, London SW7 2AZ, United Kingdom
| | - G C Rowland
- Blackett Laboratory, Imperial College London, London SW7 2AZ, United Kingdom
| | - R A Smith
- Blackett Laboratory, Imperial College London, London SW7 2AZ, United Kingdom
| | - A Frank
- Department of Physics and Astronomy, University of Rochester, Rochester, New York 14627, USA
| | - P Hartigan
- Department of Physics and Astronomy, Rice University, Houston, Texas 77005-1892, USA
| | - A L Velikovich
- Plasma Physics Division, U.S. Naval Research Laboratory, Washington, DC 20375, USA
| | - J P Chittenden
- Blackett Laboratory, Imperial College London, London SW7 2AZ, United Kingdom
| | - S V Lebedev
- Blackett Laboratory, Imperial College London, London SW7 2AZ, United Kingdom
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2
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Simon Wedlund C, Volwerk M, Beth A, Mazelle C, Möstl C, Halekas J, Gruesbeck JR, Rojas‐Castillo D. A Fast Bow Shock Location Predictor-Estimator From 2D and 3D Analytical Models: Application to Mars and the MAVEN Mission. JOURNAL OF GEOPHYSICAL RESEARCH. SPACE PHYSICS 2022; 127:e2021JA029942. [PMID: 35865029 PMCID: PMC9285960 DOI: 10.1029/2021ja029942] [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: 09/06/2021] [Revised: 11/30/2021] [Accepted: 12/21/2021] [Indexed: 06/15/2023]
Abstract
We present fast algorithms to automatically estimate the statistical position of the bow shock from spacecraft data, using existing analytical two-dimensional (2D) and three-dimensional (3D) models of the shock surface. We derive expressions of the standoff distances in 2D and 3D and of the normal to the bow shock at any given point on it. Two simple bow shock detection algorithms are constructed, one solely based on a geometrical predictor from existing models, the other using this predicted position to further refine it with the help of magnetometer data, an instrument flown on many planetary missions. Both empirical techniques are applicable to any planetary environment with a defined shock structure. Applied to the Martian environment and the NASA/MAVEN mission, the predicted shock position is on average within 0.15 planetary radius R p of the bow shock crossing. Using the predictor-corrector algorithm, this estimate is further refined to within a few minutes of the true crossing (≈0.05R p). Between 2014 and 2021, we detect 14,929 clear bow shock crossings, predominantly quasi-perpendicular. Thanks to 2D conic and 3D quadratic fits, we investigate the variability of the shock surface with respect to Mars Years (MY), solar longitude (Ls), and solar EUV flux levels. Although asymmetry in Y and Z Mars Solar Orbital coordinates is on average small, we show that for MY32 and MY35, Ls = [135°-225°] and high solar flux, it can become particularly noticeable, and is superimposed to the usual North-South asymmetry due in part to the presence of crustal magnetic fields.
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Affiliation(s)
| | - Martin Volwerk
- Space Research InstituteAustrian Academy of SciencesGrazAustria
| | - Arnaud Beth
- Department of PhysicsUmeå UniversityUmeåSweden
| | - Christian Mazelle
- Institut de Recherche en Astrophysique et PlanétologieUniversité de ToulouseCNRSUPSCNESToulouseFrance
| | - Christian Möstl
- Space Research InstituteAustrian Academy of SciencesGrazAustria
| | - Jasper Halekas
- Department of Physics and AstronomyUniversity of IowaIowa CityIAUSA
| | - Jacob R. Gruesbeck
- NASA Goddard Space Flight CenterLaboratory for Planetary MagnetospheresGreenbeltMDUSA
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3
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Mostafavi P, Burlaga LF, Cairns IH, Fuselier SA, Fraternale F, Gurnett DA, Kim TK, Kurth WS, Pogorelov NV, Provornikova E, Richardson JD, Turner DL, Zank GP. Shocks in the Very Local Interstellar Medium. SPACE SCIENCE REVIEWS 2022; 218:27. [PMID: 35574274 PMCID: PMC9085707 DOI: 10.1007/s11214-022-00893-4] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/16/2022] [Accepted: 04/15/2022] [Indexed: 05/08/2023]
Abstract
Large-scale disturbances generated by the Sun's dynamics first propagate through the heliosphere, influence the heliosphere's outer boundaries, and then traverse and modify the very local interstellar medium (VLISM). The existence of shocks in the VLISM was initially suggested by Voyager observations of the 2-3 kHz radio emissions in the heliosphere. A couple of decades later, both Voyagers crossed the definitive edge of our heliosphere and became the first ever spacecraft to sample interstellar space. Since Voyager 1's entrance into the VLISM, it sampled electron plasma oscillation events that indirectly measure the medium's density, increasing as it moves further away from the heliopause. Some of the observed electron oscillation events in the VLISM were associated with the local heliospheric shock waves. The observed VLISM shocks were very different than heliospheric shocks. They were very weak and broad, and the usual dissipation via wave-particle interactions could not explain their structure. Estimates of the dissipation associated with the collisionality show that collisions can determine the VLISM shock structure. According to theory and models, the existence of a bow shock or wave in front of our heliosphere is still an open question as there are no direct observations yet. This paper reviews the outstanding observations recently made by the Voyager 1 and 2 spacecraft, and our current understanding of the properties of shocks/waves in the VLISM. We present some of the most exciting open questions related to the VLISM and shock waves that should be addressed in the future.
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Affiliation(s)
- P. Mostafavi
- Johns Hopkins Applied Physics Laboratory, Laurel, MD 20723 USA
| | - L. F. Burlaga
- NASA Goddard Space Flight Center, Code 673, Greenbelt, MD 20771 USA
| | - I. H. Cairns
- School of Physics, University of Sydney, Sydney, NSW 2006 Australia
| | - S. A. Fuselier
- Southwest Research Institute, P.O. Drawer 28510, San Antonio, TX 78228 USA
- Department of Physics and Astronomy, University of Texas at San Antonio, San Antonio, TX 78249 USA
| | - F. Fraternale
- Center for Space Plasma and Aeronomic Research (CSPAR), University of Alabama in Huntsville, Huntsville, AL 35805 USA
| | - D. A. Gurnett
- Department of Physics and Astronomy, University of Iowa, Iowa City, IA 52242 USA
| | - T. K. Kim
- Center for Space Plasma and Aeronomic Research (CSPAR), University of Alabama in Huntsville, Huntsville, AL 35805 USA
| | - W. S. Kurth
- Department of Physics and Astronomy, University of Iowa, Iowa City, IA 52242 USA
| | - N. V. Pogorelov
- Center for Space Plasma and Aeronomic Research (CSPAR), University of Alabama in Huntsville, Huntsville, AL 35805 USA
- Department of Space Science, University of Alabama in Huntsville, Huntsville, AL 35805 USA
| | - E. Provornikova
- Johns Hopkins Applied Physics Laboratory, Laurel, MD 20723 USA
| | - J. D. Richardson
- Kavli Institute for Astrophysics and Space Research, Cambridge, MA USA
- Department of Physics, Massachusetts Institute of Technology, Cambridge, MA USA
| | - D. L. Turner
- Johns Hopkins Applied Physics Laboratory, Laurel, MD 20723 USA
| | - G. P. Zank
- Center for Space Plasma and Aeronomic Research (CSPAR), University of Alabama in Huntsville, Huntsville, AL 35805 USA
- Department of Space Science, University of Alabama in Huntsville, Huntsville, AL 35805 USA
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Romanelli N, DiBraccio GA. Occurrence rate of ultra-low frequency waves in the foreshock of Mercury increases with heliocentric distance. Nat Commun 2021; 12:6748. [PMID: 34799552 PMCID: PMC8604978 DOI: 10.1038/s41467-021-26344-2] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/27/2021] [Accepted: 10/01/2021] [Indexed: 11/25/2022] Open
Abstract
Studies of Mercury's foreshock have analyzed in detail the properties of ultra-low frequency waves. However, an open question remains in regards to understanding favorable conditions for these planetary foreshocks waves. Here, we report that 0.05-0.41 Hz quasi-monochromatic waves are mostly present under quasi-radial and relatively low intensity Interplanetary Magnetic Field, based on 17 Mercury years of MESSENGER Magnetometer data. These conditions are consistent with larger foreshock size and reflection of solar wind protons, their most likely source. Consequently, we find that the wave occurrence rate increases with Mercury's heliocentric distance. Detection of these waves throughout Mercury's highly eccentric orbit suggests the conditions for backstreaming protons are potentially present for all of Mercury's heliocentric distances, despite the relatively low solar wind Alfvén Mach number regime. These results are relevant for planetary magnetospheres throughout the solar system, and the magnetospheres of exoplanets, and provide knowledge of particle acceleration mechanisms occurring inside foreshocks.
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Affiliation(s)
- N. Romanelli
- grid.164295.d0000 0001 0941 7177Department of Astronomy, University of Maryland, College Park, MD USA ,grid.133275.10000 0004 0637 6666Planetary Magnetospheres Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD USA ,grid.266673.00000 0001 2177 1144Center for Space Sciences and Technology, University of Maryland, Baltimore County, Baltimore, MD USA ,grid.133275.10000 0004 0637 6666Center for Research and Exploration in Space Science and Technology II, NASA/GSFC, Greenbelt, MD USA
| | - G. A. DiBraccio
- grid.133275.10000 0004 0637 6666Planetary Magnetospheres Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD USA
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5
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Wilson LB, Chen LJ, Wang S, Schwartz SJ, Turner DL, Stevens ML, Kasper JC, Osmane A, Caprioli D, Bale SD, Pulupa MP, Salem CS, Goodrich KA. Electron Energy Partition across Interplanetary Shocks. I. Methodology and Data Product. THE ASTROPHYSICAL JOURNAL. SUPPLEMENT SERIES 2019; 243:10.3847/1538-4365/ab22bd. [PMID: 31806920 PMCID: PMC6894189 DOI: 10.3847/1538-4365/ab22bd] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/01/2023]
Abstract
Analyses of 15,314 electron velocity distribution functions (VDFs) within ±2 hr of 52 interplanetary (IP) shocks observed by the Wind spacecraft near 1 au are introduced. The electron VDFs are fit to the sum of three model functions for the cold dense core, hot tenuous halo, and field-aligned beam/strahl component. The best results were found by modeling the core as either a bi-kappa or a symmetric (or asymmetric) bi-self-similar VDF, while both the halo and beam/strahl components were best fit to bi-kappa VDF. This is the first statistical study to show that the core electron distribution is better fit to a self-similar VDF than a bi-Maxwellian under all conditions. The self-similar distribution deviation from a Maxwellian is a measure of inelasticity in particle scattering from waves and/or turbulence. The ranges of values defined by the lower and upper quartiles for the kappa exponents are κ ec ~ 5.40-10.2 for the core, κ eh ~ 3.58-5.34 for the halo, and κ eb ~ 3.40-5.16 for the beam/strahl. The lower-to-upper quartile range of symmetric bi-self-similar core exponents is s ec ~ 2.00-2.04, and those of asymmetric bi-self-similar core exponents are p ec ~ 2.20-4.00 for the parallel exponent and q ec ~ 2.00-2.46 for the perpendicular exponent. The nuanced details of the fit procedure and description of resulting data product are also presented. The statistics and detailed analysis of the results are presented in Paper II and Paper III of this three-part study.
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Affiliation(s)
- Lynn B Wilson
- NASA Goddard Space Flight Center, Heliophysics Science Division, Greenbelt, MD, USA
| | - Li-Jen Chen
- NASA Goddard Space Flight Center, Heliophysics Science Division, Greenbelt, MD, USA
| | - Shan Wang
- NASA Goddard Space Flight Center, Heliophysics Science Division, Greenbelt, MD, USA
- Astronomy Department, University of Maryland, College Park, Maryland, USA
| | - Steven J Schwartz
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, Boulder, CO, USA
| | - Drew L Turner
- Space Sciences Department, The Aerospace Corporation, El Segundo, CA, USA
| | - Michael L Stevens
- Harvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA, USA
| | - Justin C Kasper
- University of Michigan, Ann Arbor, School of Climate and Space Sciences and Engineering, Ann Arbor, MI, USA
| | - Adnane Osmane
- Department of Physics, University of Helsinki, Helsinki, Finland
| | - Damiano Caprioli
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA
| | - Stuart D Bale
- University of California Berkeley, Space Sciences Laboratory, Berkeley, CA, USA
| | - Marc P Pulupa
- University of California Berkeley, Space Sciences Laboratory, Berkeley, CA, USA
| | - Chadi S Salem
- University of California Berkeley, Space Sciences Laboratory, Berkeley, CA, USA
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6
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Dimmock AP, Russell CT, Sagdeev RZ, Krasnoselskikh V, Walker SN, Carr C, Dandouras I, Escoubet CP, Ganushkina N, Gedalin M, Khotyaintsev YV, Aryan H, Pulkkinen TI, Balikhin MA. Direct evidence of nonstationary collisionless shocks in space plasmas. SCIENCE ADVANCES 2019; 5:eaau9926. [PMID: 30820454 PMCID: PMC6392793 DOI: 10.1126/sciadv.aau9926] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 08/10/2018] [Accepted: 01/17/2019] [Indexed: 06/09/2023]
Abstract
Collisionless shocks are ubiquitous throughout the universe: around stars, supernova remnants, active galactic nuclei, binary systems, comets, and planets. Key information is carried by electromagnetic emissions from particles accelerated by high Mach number collisionless shocks. These shocks are intrinsically nonstationary, and the characteristic physical scales responsible for particle acceleration remain unknown. Quantifying these scales is crucial, as it affects the fundamental process of redistributing upstream plasma kinetic energy into other degrees of freedom-particularly electron thermalization. Direct in situ measurements of nonstationary shock dynamics have not been reported. Thus, the model that best describes this process has remained unknown. Here, we present direct evidence demonstrating that the transition to nonstationarity is associated with electron-scale field structures inside the shock ramp.
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Affiliation(s)
- Andrew P. Dimmock
- Swedish Institute of Space Physics, P.O. Box 537, SE-751 21 Uppsala, Sweden
| | - Christopher T. Russell
- Department of Earth Planetary and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095, USA
| | - Roald Z. Sagdeev
- Department of Physics, University of Maryland, College Park, MD 20742, USA
| | - Vladimir Krasnoselskikh
- LPC2E, CNRS-University of Orleans, Orleans, France
- Space Sciences Laboratory at University of California, 7 Gauss Way, Berkeley, CA 94720, USA
| | - Simon N. Walker
- Department of Automatic Control and Systems Engineering, University of Sheffield, Sheffield, UK
| | | | | | - C. Philippe Escoubet
- European Space Agency/European Space Research and Technology Centre (ESA/ESTEC), Noordwijk, Netherlands
| | - Natalia Ganushkina
- Finnish Meteorological Institute, Helsinki, Finland
- University of Michigan, Ann Arbor, MI 48109, USA
| | - Michael Gedalin
- Department of Physics, Ben-Gurion University, Beer-Sheva, Israel
| | | | - Homayon Aryan
- Department of Automatic Control and Systems Engineering, University of Sheffield, Sheffield, UK
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Tuija I. Pulkkinen
- University of Michigan, Ann Arbor, MI 48109, USA
- Department of Electronics and Nanoengineering, School of Electrical Engineering, Aalto University, Espoo, Finland
| | - Michael A. Balikhin
- Department of Automatic Control and Systems Engineering, University of Sheffield, Sheffield, UK
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7
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Wilson LB, Koval A, Szabo A, Stevens ML, Kasper JC, Cattell CA, Krasnoselskikh VV. Revisiting the structure of low-Mach number, low-beta, quasi-perpendicular shocks. JOURNAL OF GEOPHYSICAL RESEARCH. SPACE PHYSICS 2017; 122:9115-9133. [PMID: 30410850 PMCID: PMC6219398 DOI: 10.1002/2017ja024352] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
A study of the structure of 145 low-Mach number (M ≤ 3), low-beta (β ≤ 1), quasi-perpendicular interplanetary collisionless shock waves observed by the Wind spacecraft has provided strong evidence that these shocks have large-amplitude whistler precursors. The common occurrence and large amplitudes of the precursors raise doubts about the standard assumption that such shocks can be classified as laminar structures. This directly contradicts standard models. In 113 of the 145 shocks (~78%), we observe clear evidence of magnetosonic-whistler precursor fluctuations with frequencies ~0.1-7 Hz. We find no dependence on the upstream plasma beta, or any other shock parameter, for the presence or absence of precursors. The majority (~66%) of the precursors propagate at ≤45° with respect to the upstream average magnetic field and most (~87%) propagate ≥30° from the shock normal vector. Further, most (~79%) of the waves propagate at least 20° from the coplanarity plane. The peak-to-peak wave amplitudes (δB pk-pk) are large with a range of maximum values for the 113 precursors of ~0.4-13 nT with an average of ~2 nT. When we normalize the wave amplitudes to the upstream averaged magnetic field and the shock ramp amplitude, we find average values of ~40% and ~220%, respectively.
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Affiliation(s)
- L B Wilson
- NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
| | - A Koval
- NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
- Goddard Planetary Heliophysics Institute, University of Maryland, Baltimore County, Baltimore, Maryland, USA
| | - A Szabo
- NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
| | - M L Stevens
- Harvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, Massachusetts, USA
| | - J C Kasper
- School of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan, USA
| | - C A Cattell
- School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota, USA
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8
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Malkov MA, Diamond PH, Sagdeev RZ. Proton-helium spectral anomaly as a signature of cosmic ray accelerator. PHYSICAL REVIEW LETTERS 2012; 108:081104. [PMID: 22463513 DOI: 10.1103/physrevlett.108.081104] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/24/2011] [Indexed: 05/31/2023]
Abstract
The much-anticipated proof of cosmic ray (CR) acceleration in supernova remnants must hinge on the full consistency of acceleration theory with the observations; direct proof is impossible because of CR-orbit scrambling. Recent observations indicate deviations between helium and proton CR rigidity spectra inconsistent with the theory. By considering an initial (injection) phase of the diffusive shock acceleration, where elemental similarity does not apply, we demonstrate that the spectral difference is, in fact, a unique signature of the acceleration mechanism. Collisionless shocks inject more He(2+) when they are stronger and so produce harder He(2+) spectra. The injection bias is due to Alfvén waves driven by the more abundant protons, so the He(2+) ions are harder to trap by these waves. By fitting the p/He ratio to the PAMELA data, we bolster the diffusive shock acceleration case for resolving the century-old mystery of CR origin.
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Affiliation(s)
- M A Malkov
- CASS and Department of Physics, University of California, San Diego, La Jolla, California 92093, USA
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9
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Dimmock AP, Balikhin MA, Krasnoselskikh VV, Walker SN, Bale SD, Hobara Y. A statistical study of the cross-shock electric potential at low Mach number, quasi-perpendicular bow shock crossings using Cluster data. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011ja017089] [Citation(s) in RCA: 30] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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10
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Sundkvist D, Krasnoselskikh V, Bale SD, Schwartz SJ, Soucek J, Mozer F. Dispersive nature of high mach number collisionless plasma shocks: Poynting flux of oblique whistler waves. PHYSICAL REVIEW LETTERS 2012; 108:025002. [PMID: 22324692 DOI: 10.1103/physrevlett.108.025002] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/28/2011] [Indexed: 05/31/2023]
Abstract
Whistler wave trains are observed in the foot region of high Mach number quasiperpendicular shocks. The waves are oblique with respect to the ambient magnetic field as well as the shock normal. The Poynting flux of the waves is directed upstream in the shock normal frame starting from the ramp of the shock. This suggests that the waves are an integral part of the shock structure with the dispersive shock as the source of the waves. These observations lead to the conclusion that the shock ramp structure of supercritical high Mach number shocks is formed as a balance of dispersion and nonlinearity.
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Affiliation(s)
- David Sundkvist
- Space Sciences Laboratory, University of California, Berkeley, California, USA.
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11
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Tiu D, Cairns IH, Yuan X, Robinson PA. Evidence for reformation of the Uranian bow shock: Hybrid simulations and comparisons with Voyager data. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010ja016057] [Citation(s) in RCA: 10] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- Dion Tiu
- School of Physics; University of Sydney; Sydney, New South Wales Australia
| | - Iver H. Cairns
- School of Physics; University of Sydney; Sydney, New South Wales Australia
| | - Xingqiu Yuan
- School of Physics; University of Sydney; Sydney, New South Wales Australia
- Geomagnetic Laboratory, Natural Resources Canada; Ottawa, Ontario Canada
| | - P. A. Robinson
- School of Physics; University of Sydney; Sydney, New South Wales Australia
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12
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Hobara Y, Balikhin M, Krasnoselskikh V, Gedalin M, Yamagishi H. Statistical study of the quasi-perpendicular shock ramp widths. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2010ja015659] [Citation(s) in RCA: 37] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Y. Hobara
- Department of Electronic Engineering and Research Station on Seismo Electromagnetics; University of Electro-Communications; Chofu Japan
- ACSE; University of Sheffield; Sheffield UK
| | | | | | - M. Gedalin
- Department of Physics; Ben-Gurion University; Beer-Sheva Israel
| | - H. Yamagishi
- National Institute of Polar Research; Tokyo Japan
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13
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Achilleos N, Bertucci C, Russell CT, Hospodarsky GB, Rymer AM, Arridge CS, Burton ME, Dougherty MK, Hendricks S, Smith EJ, Tsurutani BT. Orientation, location, and velocity of Saturn's bow shock: Initial results from the Cassini spacecraft. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005ja011297] [Citation(s) in RCA: 48] [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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14
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15
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Balikhin MA, Nozdrachev M, Dunlop M, Krasnosel'skikh V, Walker SN, Alleyne HSCK, Formisano V, Andre M, Balogh A, Eriksson A, Yearby K. Observation of the terrestrial bow shock in quasi-electrostatic subshock regime. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2001ja000327] [Citation(s) in RCA: 20] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- M. A. Balikhin
- Space Instrumentation Group, Department of Automatic Control and Systems Engineering; University of Sheffield; Sheffield UK
| | - M. Nozdrachev
- Space Instrumentation Group, Department of Automatic Control and Systems Engineering; University of Sheffield; Sheffield UK
| | - M. Dunlop
- Blackett Laboratory; Imperial College of Science, Technology and Medicine; London UK
| | - V. Krasnosel'skikh
- Laboratoire de Physique et Chimie de l'Environnement, CNRS; Orleans France
| | - S. N. Walker
- Space Instrumentation Group, Department of Automatic Control and Systems Engineering; University of Sheffield; Sheffield UK
| | - H. St. C. K. Alleyne
- Space Instrumentation Group, Department of Automatic Control and Systems Engineering; University of Sheffield; Sheffield UK
| | - V. Formisano
- Consiglio Nazionale delle Richerche; Frascati Italy
| | - M. Andre
- Consiglio Nazionale delle Richerche; Frascati Italy
| | - A. Balogh
- Blackett Laboratory; Imperial College of Science, Technology and Medicine; London UK
| | - A. Eriksson
- Swedish Institute of Space Physics-Uppsala; Uppsala Sweden
| | - K. Yearby
- Space Instrumentation Group, Department of Automatic Control and Systems Engineering; University of Sheffield; Sheffield UK
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16
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Tsurutani BT, Smith EJ, Burton ME, Arballo JK, Galvan C, Zhou XY, Southwood DJ, Dougherty MK, Glassmeier KH, Neubauer FM, Chao JK. Oblique “1-Hz” whistler mode waves in an electron foreshock: The Cassini near-Earth encounter. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2001ja900108] [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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17
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Tátrallyay M, Gévai G, Apáthy I, Schwingenschuh K, Zhang TL, Kotova GA, Verigin MI, Livi S, Rosenbauer H. Magnetic field overshoots in the Martian bow shock. ACTA ACUST UNITED AC 1997. [DOI: 10.1029/96ja00073] [Citation(s) in RCA: 13] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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