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Miyoshi Y, Shinohara I, Ukhorskiy S, Claudepierre SG, Mitani T, Takashima T, Hori T, Santolik O, Kolmasova I, Matsuda S, Kasahara Y, Teramoto M, Katoh Y, Hikishima M, Kojima H, Kurita S, Imajo S, Higashio N, Kasahara S, Yokota S, Asamura K, Kazama Y, Wang SY, Jun CW, Kasaba Y, Kumamoto A, Tsuchiya F, Shoji M, Nakamura S, Kitahara M, Matsuoka A, Shiokawa K, Seki K, Nosé M, Takahashi K, Martinez-Calderon C, Hospodarsky G, Colpitts C, Kletzing C, Wygant J, Spence H, Baker DN, Reeves GD, Blake JB, Lanzerotti L. Collaborative Research Activities of the Arase and Van Allen Probes. Space Sci Rev 2022; 218:38. [PMID: 35757012 PMCID: PMC9213325 DOI: 10.1007/s11214-022-00885-4] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 08/17/2021] [Accepted: 03/23/2022] [Indexed: 06/15/2023]
Abstract
This paper presents the highlights of joint observations of the inner magnetosphere by the Arase spacecraft, the Van Allen Probes spacecraft, and ground-based experiments integrated into spacecraft programs. The concurrent operation of the two missions in 2017-2019 facilitated the separation of the spatial and temporal structures of dynamic phenomena occurring in the inner magnetosphere. Because the orbital inclination angle of Arase is larger than that of Van Allen Probes, Arase collected observations at higher L -shells up to L ∼ 10 . After March 2017, similar variations in plasma and waves were detected by Van Allen Probes and Arase. We describe plasma wave observations at longitudinally separated locations in space and geomagnetically-conjugate locations in space and on the ground. The results of instrument intercalibrations between the two missions are also presented. Arase continued its normal operation after the scientific operation of Van Allen Probes completed in October 2019. The combined Van Allen Probes (2012-2019) and Arase (2017-present) observations will cover a full solar cycle. This will be the first comprehensive long-term observation of the inner magnetosphere and radiation belts.
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Affiliation(s)
- Y. Miyoshi
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, 464-8601 Japan
| | - I. Shinohara
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, 252-5210 Japan
| | - S. Ukhorskiy
- Applied Physics Laboratory, The Johns Hopkins University, 11101 Johns Hopkins Rd, Laurel, MD 20723 USA
| | - S. G. Claudepierre
- Department of Atmospheric and Oceanic Sciences, University of California, Los Angeles, 7115 Math Sciences Bldg., Los Angeles, CA 90095 USA
| | - T. Mitani
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, 252-5210 Japan
| | - T. Takashima
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, 252-5210 Japan
| | - T. Hori
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, 464-8601 Japan
| | - O. Santolik
- Faculty of Mathematics an Physics, Charles University, V Holesovickach 2, 18000 Prague, Czechia
- Dept. of Space Physics, Institute of Atmospheric Physics, Czech Academy of Sciences, Bocni II 1401, 14100 Prague, Czechia
| | - I. Kolmasova
- Faculty of Mathematics an Physics, Charles University, V Holesovickach 2, 18000 Prague, Czechia
- Dept. of Space Physics, Institute of Atmospheric Physics, Czech Academy of Sciences, Bocni II 1401, 14100 Prague, Czechia
| | - S. Matsuda
- Graduate School of Natural Science and Technology, Kanazawa University, Kanazawa, 920-1192 Japan
| | - Y. Kasahara
- Graduate School of Natural Science and Technology, Kanazawa University, Kanazawa, 920-1192 Japan
| | - M. Teramoto
- Graduate School of Engineering, Kyushu Institute of Technology, Kitakyusyu, 804-8550 Japan
| | - Y. Katoh
- Graduate School of Science, Tohoku University, Sendai, 980-8578 Japan
| | - M. Hikishima
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, 252-5210 Japan
| | - H. Kojima
- Research Institute for Sustainable Humanosphere, Kyoto University, Uji, 611-0011 Japan
| | - S. Kurita
- Research Institute for Sustainable Humanosphere, Kyoto University, Uji, 611-0011 Japan
| | - S. Imajo
- Graduate School of Science, Kyoto University, Kyoto, 606-8502 Japan
| | - N. Higashio
- Strategic Planning and Management Department, Japan Aerospace Exploration Agency, Tokyo, 101-8008 Japan
| | - S. Kasahara
- Graduate School of Science, University of Tokyo, Tokyo, 113-0033 Japan
| | - S. Yokota
- Graduate School of Science, Osaka University, Toyonaka, 560-0043 Japan
| | - K. Asamura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, 252-5210 Japan
| | - Y. Kazama
- Institute of Astronomy and Astrophysics, Academia Sinica, No. 1, Sec. 4, Roosevelt Rd, Taipei, 10617 Taiwan
| | - S.-Y. Wang
- Institute of Astronomy and Astrophysics, Academia Sinica, No. 1, Sec. 4, Roosevelt Rd, Taipei, 10617 Taiwan
| | - C.-W. Jun
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, 464-8601 Japan
| | - Y. Kasaba
- Graduate School of Science, Tohoku University, Sendai, 980-8578 Japan
| | - A. Kumamoto
- Graduate School of Science, Tohoku University, Sendai, 980-8578 Japan
| | - F. Tsuchiya
- Graduate School of Science, Tohoku University, Sendai, 980-8578 Japan
| | - M. Shoji
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, 464-8601 Japan
| | - S. Nakamura
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, 464-8601 Japan
- Institute for Advanced Research, Nagoya University, Nagoya, 464-8601 Japan
| | - M. Kitahara
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, 464-8601 Japan
- Graduate School of Science, Tohoku University, Sendai, 980-8578 Japan
| | - A. Matsuoka
- Graduate School of Science, Kyoto University, Kyoto, 606-8502 Japan
| | - K. Shiokawa
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, 464-8601 Japan
| | - K. Seki
- Graduate School of Science, University of Tokyo, Tokyo, 113-0033 Japan
| | - M. Nosé
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, 464-8601 Japan
| | - K. Takahashi
- Applied Physics Laboratory, The Johns Hopkins University, 11101 Johns Hopkins Rd, Laurel, MD 20723 USA
| | - C. Martinez-Calderon
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, 464-8601 Japan
| | - G. Hospodarsky
- Department of Physics and Astronomy, University of Iowa, Van Allen Hall (VAN), Iowa City, IA 52242 USA
| | - C. Colpitts
- School of Physics and Astronomy, University of Minnesota, 116 Church St. SE, Minneapolis, MN 55455 USA
| | - Craig Kletzing
- Department of Physics and Astronomy, University of Iowa, Van Allen Hall (VAN), Iowa City, IA 52242 USA
| | - J. Wygant
- School of Physics and Astronomy, University of Minnesota, 116 Church St. SE, Minneapolis, MN 55455 USA
| | - H. Spence
- Institute for the Study of Earth, Oceans, and Space, University of New Hampshire, 8 College Road, Durham, NH 03824 USA
| | - D. N. Baker
- Laboratory for Atmospheric and Space Physics, University of Colorado, 3665 Discovery Drive, 600 UCB, Boulder, CO 80303 USA
| | - G. D. Reeves
- Inteligence & Space Reserarch Division, Los Alamos National Laboratory, PO Box 1663, Los Alamos, NM USA
| | - J. B. Blake
- The Aerospace Corporation, P.O. Box 92957, Los Angeles, CA 90009-2957 USA
| | - L. Lanzerotti
- Department of Physics, New Jersey Institute of Technology, Newark, NJ 07102 USA
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Takahashi K, Crabtree C, Ukhorskiy AY, Boyd A, Denton RE, Turner D, Gkioulidou M, Vellante M, Spence HE. Van Allen Probes Observations of Symmetric Stormtime Compressional ULF Waves. J Geophys Res Space Phys 2022; 127:e2021JA030115. [PMID: 35847659 PMCID: PMC9285050 DOI: 10.1029/2021ja030115] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 11/08/2021] [Revised: 12/16/2021] [Accepted: 01/23/2022] [Indexed: 06/15/2023]
Abstract
Previous spacecraft studies showed that stormtime poloidal ultralow-frequency (ULF) waves in the ring current region have an antisymmetric (second harmonic) mode structure about the magnetic equator. This paper reports Van Allen Probes observations of symmetric ULF waves in the postnoon sector during a moderate geomagnetic storm. The mode structure is determined from the presence of purely compressional magnetic field oscillations at the equator accompanied by strong transverse electric field perturbations. Antisymmetric waves were also detected but only very late in the recovery phase. The symmetric waves were detected outside the plasmasphere at L = 3.0-5.5 and had peak power at 4-10 mHz, lower than the frequency of the local fundamental toroidal standing Alfvén wave. During the wave events, the flux of protons was enhanced at energies below ∼5 keV, which appears to be a prerequisite for the waves. The protons may provide free energies to waves through drift resonance instability or drift compressional instability, which occur in the presence of radial gradients of plasma parameters.
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Affiliation(s)
- Kazue Takahashi
- The Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | | | - A. Y. Ukhorskiy
- The Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - Alexander Boyd
- Department of Space ScienceAerospace CorporationChantillyVAUSA
| | | | - Drew Turner
- The Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | | | - Massimo Vellante
- Department of Physical and Chemical SciencesUniversity of L’AquilaL’AquilaItaly
- Consorzio Area di Ricerca in AstrogeofisicaL’AquilaItaly
| | - Harlan E. Spence
- Institute for the Study of Earth, Oceans, and Space, University of New HampshireDurhamNHUSA
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Vellante M, Takahashi K, Del Corpo A, Zhelavskaya IS, Goldstein J, Mann IR, Pietropaolo E, Reda J, Heilig B. Multi-Instrument Characterization of Magnetospheric Cold Plasma Dynamics in the June 22, 2015 Geomagnetic Storm. J Geophys Res Space Phys 2021; 126:e2021JA029292. [PMID: 34434688 PMCID: PMC8365745 DOI: 10.1029/2021ja029292] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 02/26/2021] [Revised: 05/06/2021] [Accepted: 05/28/2021] [Indexed: 06/13/2023]
Abstract
We present a comparison of magnetospheric plasma mass/electron density observations during an 11-day interval which includes the geomagnetic storm of June 22, 2015. For this study we used: Equatorial plasma mass density derived from geomagnetic field line resonances (FLRs) detected by Van Allen Probes and at the ground-based magnetometer networks EMMA and CARISMA; in situ electron density inferred by the Neural-network-based Upper hybrid Resonance Determination algorithm applied to plasma wave Van Allen Probes measurements. The combined observations at L ∼ 4, MLT ∼ 16 of the two longitudinally separated magnetometer networks show a temporal pattern very similar to that of the in situ observations: A density decrease by an order of magnitude about 1 day after the Dst minimum, a partial recovery a few hours later, and a new strong decrease soon after. The observations are consistent with the position of the measurement points with respect to the plasmasphere boundary as derived by a plasmapause test particle simulation. A comparison between plasma mass densities derived from ground and in situ FLR observations during favorable conjunctions shows a good agreement. We find however, for L < ∼3, the spacecraft measurements to be higher than the corresponding ground observations with increasing deviation with decreasing L, which might be related to the rapid outbound spacecraft motion in that region. A statistical analysis of the average ion mass using simultaneous spacecraft measurements of mass and electron density indicates values close to 1 amu in plasmasphere and higher values (∼2-3 amu) in plasmatrough.
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Affiliation(s)
- M. Vellante
- Department of Physical and Chemical SciencesUniversity of L'AquilaL'AquilaItaly
| | - K. Takahashi
- The Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - A. Del Corpo
- Department of Physical and Chemical SciencesUniversity of L'AquilaL'AquilaItaly
| | - I. S. Zhelavskaya
- Helmholtz Centre PotsdamGFZ German Research Centre for Geosciences and University of PotsdamPotsdamGermany
| | - J. Goldstein
- Space Science and Engineering DivisionSouthwest Research InstituteSan AntonioTXUSA
| | | | - E. Pietropaolo
- Department of Physical and Chemical SciencesUniversity of L'AquilaL'AquilaItaly
| | - J. Reda
- Institute of GeophysicsPolish Academy of SciencesWarsawPoland
| | - B. Heilig
- Mining and Geological Survey of HungaryBudapestHungary
- Eötvös Loránd UniversityBudapestHungary
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4
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Boyd AJ, Reeves GD, Spence HE, Funsten HO, Larsen BA, Skoug RM, Blake JB, Fennell JF, Claudepierre SG, Baker DN, Kanekal SG, Jaynes AN. RBSP-ECT Combined Spin-Averaged Electron Flux Data Product. J Geophys Res Space Phys 2019; 124:9124-9136. [PMID: 32025458 PMCID: PMC6988469 DOI: 10.1029/2019ja026733] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 03/20/2019] [Revised: 08/19/2019] [Accepted: 08/27/2019] [Indexed: 06/10/2023]
Abstract
We describe a new data product combining the spin-averaged electron flux measurements from the Radiation Belt Storm Probes (RBSP) Energetic Particle Composition and Thermal Plasma (ECT) suite on the National Aeronautics and Space Administration's Van Allen Probes. We describe the methodology used to combine each of the data sets and produce a consistent set of spectra for September 2013 to the present. Three-minute-averaged flux spectra are provided spanning energies from 15 eV up to 20 MeV. This new data product provides additional utility to the ECT data and offers a consistent cross calibrated data set for researchers interested in examining the dynamics of the inner magnetosphere across a wide range of energies.
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Affiliation(s)
| | - G. D. Reeves
- New Mexico ConsortiumLos AlamosNMUSA
- Los Alamos National LaboratoryLos AlamosNMUSA
| | - H. E. Spence
- Institute for the Study of Earth, Oceans and SpaceUniversity of New HampshireDurhamNHUSA
| | | | - B. A. Larsen
- New Mexico ConsortiumLos AlamosNMUSA
- Los Alamos National LaboratoryLos AlamosNMUSA
| | - R. M. Skoug
- Los Alamos National LaboratoryLos AlamosNMUSA
| | | | | | - S. G. Claudepierre
- The Aerospace CorporationEl SegundoCAUSA
- Department of Atmospheric and Oceanic SciencesUniversity of CaliforniaLos AngelesCAUSA
| | - D. N. Baker
- Laboratory for Atmospheric and Space SciencesUniversity of Colorado BoulderBoulderCOUSA
| | | | - A. N. Jaynes
- Department of Physics and AstronomyUniversity of IowaIowa CityIAUSA
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5
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Baker DN, Hoxie V, Zhao H, Jaynes AN, Kanekal S, Li X, Elkington S. Multiyear Measurements of Radiation Belt Electrons: Acceleration, Transport, and Loss. J Geophys Res Space Phys 2019; 124:2588-2602. [PMID: 31245234 PMCID: PMC6582599 DOI: 10.1029/2018ja026259] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 11/14/2018] [Revised: 12/21/2018] [Accepted: 01/03/2019] [Indexed: 06/09/2023]
Abstract
In addition to clarifying morphological structures of the Earth's radiation belts, it has also been a major achievement of the Van Allen Probes mission to understand more thoroughly how highly relativistic and ultrarelativistic electrons are accelerated deep inside the radiation belts. Prior studies have demonstrated that electrons up to energies of 10 megaelectron volts (MeV) can be produced over broad regions of the outer Van Allen zone on timescales of minutes to a few hours. It often is seen that geomagnetic activity driven by strong solar storms (i.e., coronal mass ejections, or CMEs) almost inexorably leads to relativistic electron production through the intermediary step of intense magnetospheric substorms. In this study, we report observations over the 6-year period 1 September 2012 to 1 September 2018. We focus on data about the relativistic and ultrarelativistic electrons (E≥5 MeV) measured by the Relativistic Electron-Proton Telescope sensors on board the Van Allen Probes spacecraft. This work portrays the radiation belt acceleration, transport, and loss characteristics over a wide range of geomagnetic events. We emphasize features seen repeatedly in the data (three-belt structures, "impenetrable" barrier properties, and radial diffusion signatures) in the context of acceleration and loss mechanisms. We especially highlight solar wind forcing of the ultrarelativistic electron populations and extended periods when such electrons were absent. The analysis includes new display tools showing spatial features of the mission-long time variability of the outer Van Allen belt emphasizing the remarkable dynamics of the system.
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Affiliation(s)
- Daniel N. Baker
- Laboratory for Atmospheric and Space PhysicsUniversity of ColoradoBoulderCOUSA
| | - Vaughn Hoxie
- Laboratory for Atmospheric and Space PhysicsUniversity of ColoradoBoulderCOUSA
| | - Hong Zhao
- Laboratory for Atmospheric and Space PhysicsUniversity of ColoradoBoulderCOUSA
| | | | | | - Xinlin Li
- Laboratory for Atmospheric and Space PhysicsUniversity of ColoradoBoulderCOUSA
| | - Scot Elkington
- Laboratory for Atmospheric and Space PhysicsUniversity of ColoradoBoulderCOUSA
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6
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Sandhu JK, Rae IJ, Freeman MP, Forsyth C, Gkioulidou M, Reeves GD, Spence HE, Jackman CM, Lam MM. Energization of the Ring Current by Substorms. J Geophys Res Space Phys 2018; 123:8131-8148. [PMID: 30775195 PMCID: PMC6360953 DOI: 10.1029/2018ja025766] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/11/2018] [Revised: 08/10/2018] [Accepted: 09/12/2018] [Indexed: 06/01/2023]
Abstract
The substorm process releases large amounts of energy into the magnetospheric system, although where the energy is transferred to and how it is partitioned remains an open question. In this study, we address whether the substorm process contributes a significant amount of energy to the ring current. The ring current is a highly variable region, and understanding the energization processes provides valuable insight into how substorm-ring current coupling may contribute to the generation of storm conditions and provide a source of energy for wave driving. In order to quantify the energy input into the ring current during the substorm process, we analyze Radiation Belt Storm Probes Ion Composition Experiment and Helium Oxygen Proton Electron ion flux measurements for H+, O+, and He+. The energy content of the ring current is estimated and binned spatially for L and magnetic local time. The results are combined with an independently derived substorm event list to perform a statistical analysis of variations in the ring current energy content with substorm phase. We show that the ring current energy is significantly higher in the expansion phase compared to the growth phase, with the energy enhancement persisting into the substorm recovery phase. The characteristics of the energy enhancement suggest the injection of energized ions from the tail plasma sheet following substorm onset. The local time variations indicate a loss of energetic H+ ions in the afternoon sector, likely due to wave-particle interactions. Overall, we find that the average energy input into the ring current is ∼9% of the previously reported energy released during substorms.
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Affiliation(s)
- J. K. Sandhu
- Department of Space and Climate Physics, Mullard Space Science LaboratoryUniversity College LondonLondonUK
| | - I. J. Rae
- Department of Space and Climate Physics, Mullard Space Science LaboratoryUniversity College LondonLondonUK
| | | | - C. Forsyth
- Department of Space and Climate Physics, Mullard Space Science LaboratoryUniversity College LondonLondonUK
| | - M. Gkioulidou
- Applied Physics LaboratoryJohns Hopkins UniversityBaltimoreMDUSA
| | | | - H. E. Spence
- Institute for the Study of Earth, Oceans, and SpaceUniversity of New HampshireDurhamNHUSA
| | - C. M. Jackman
- Department of Physics and AstronomyUniversity of SouthamptonSouthamptonUK
| | - M. M. Lam
- Department of Physics and AstronomyUniversity of SouthamptonSouthamptonUK
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7
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Fernandes PA, Larsen BA, Thomsen MF, Skoug RM, Reeves GD, Denton MH, Friedel RHW, Funsten HO, Goldstein J, Henderson MG, Jahn J, MacDonald EA, Olson DK. The plasma environment inside geostationary orbit: A Van Allen Probes HOPE survey. J Geophys Res Space Phys 2017; 122:9207-9227. [PMID: 29214118 PMCID: PMC5703442 DOI: 10.1002/2017ja024160] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 03/16/2017] [Revised: 07/25/2017] [Accepted: 08/14/2017] [Indexed: 06/07/2023]
Abstract
The two full precessions in local time completed by the Van Allen Probes enable global specification of the near-equatorial inner magnetosphere plasma environment. Observations by the Helium-Oxygen-Proton-Electron (HOPE) mass spectrometers provide detailed insight into the global spatial distribution of electrons, H+, He+, and O+. Near-equatorial omnidirectional fluxes and abundance ratios at energies 0.1-30 keV are presented for 2 ≤ L ≤ 6 as a function of L shell, magnetic local time (MLT), and geomagnetic activity. We present a new tool built on the UBK modeling technique for classifying plasma sheet particle access to the inner magnetosphere. This new tool generates access maps for particles of constant energy for more direct comparison with in situ measurements, rather than the traditional constant μ presentation typically associated with UBK. We present for the first time inner magnetosphere abundances of O+ flux relative to H+ flux as a function of Kp, L, MLT, and energy. At L = 6, the O+/H+ ratio increases with increasing Kp, consistent with previous results. However, at L < 5 the O+/H+ ratio generally decreases with increasing Kp. We identify a new "afternoon bulge" plasma population enriched in 10 keV O+ and superenriched in 10 keV He+ that is present during quiet/moderate geomagnetic activity (Kp < 5) at ~1100-2000 MLT and L shell 2-4. Drift path modeling results are consistent with the narrow energy and approximate MLT location of this enhancement, but the underlying physics describing its formation, structure, and depletion during higher geomagnetic activity are currently not understood.
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Affiliation(s)
- Philip A. Fernandes
- ISR‐1, Los Alamos National LaboratoryLos AlamosNew MexicoUSA
- New Mexico ConsortiumLos AlamosNew MexicoUSA
| | - Brian A. Larsen
- ISR‐1, Los Alamos National LaboratoryLos AlamosNew MexicoUSA
- New Mexico ConsortiumLos AlamosNew MexicoUSA
| | | | - Ruth M. Skoug
- ISR‐1, Los Alamos National LaboratoryLos AlamosNew MexicoUSA
- New Mexico ConsortiumLos AlamosNew MexicoUSA
| | - Geoffrey D. Reeves
- ISR‐1, Los Alamos National LaboratoryLos AlamosNew MexicoUSA
- New Mexico ConsortiumLos AlamosNew MexicoUSA
| | - Michael H. Denton
- New Mexico ConsortiumLos AlamosNew MexicoUSA
- Space Science InstituteBoulderColoradoUSA
| | - Reinhard H. W. Friedel
- New Mexico ConsortiumLos AlamosNew MexicoUSA
- CSES, Los Alamos National LaboratoryLos AlamosNew MexicoUSA
| | | | - Jerry Goldstein
- Department of Space ScienceSouthwest Research InstituteSan AntonioTexasUSA
| | - Michael G. Henderson
- ISR‐1, Los Alamos National LaboratoryLos AlamosNew MexicoUSA
- New Mexico ConsortiumLos AlamosNew MexicoUSA
| | - Jörg‐Micha Jahn
- Department of Space ScienceSouthwest Research InstituteSan AntonioTexasUSA
| | | | - David K. Olson
- ISR‐1, Los Alamos National LaboratoryLos AlamosNew MexicoUSA
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8
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Sarno-Smith LK, Larsen BA, Skoug RM, Liemohn MW, Breneman A, Wygant JR, Thomsen MF. Spacecraft surface charging within geosynchronous orbit observed by the Van Allen Probes. Space Weather 2016; 14:151-164. [PMID: 27398076 PMCID: PMC4933096 DOI: 10.1002/2015sw001345] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 11/20/2015] [Revised: 01/21/2016] [Accepted: 02/03/2016] [Indexed: 06/06/2023]
Abstract
Using the Helium Oxygen Proton Electron (HOPE) and Electric Field and Waves (EFW) instruments from the Van Allen Probes, we explored the relationship between electron energy fluxes in the eV and keV ranges and spacecraft surface charging. We present statistical results on spacecraft charging within geosynchronous orbit by L and MLT. An algorithm to extract the H+ charging line in the HOPE instrument data was developed to better explore intense charging events. Also, this study explored how spacecraft potential relates to electron number density, electron pressure, electron temperature, thermal electron current, and low-energy ion density between 1 and 210 eV. It is demonstrated that it is imperative to use both EFW potential measurements and the HOPE instrument ion charging line for examining times of extreme spacecraft charging of the Van Allen Probes. The results of this study show that elevated electron energy fluxes and high-electron pressures are present during times of spacecraft charging but these same conditions may also occur during noncharging times. We also show noneclipse significant negative charging events on the Van Allen Probes.
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Affiliation(s)
- Lois K Sarno-Smith
- Department of Climate and Space Engineering University of Michigan Ann Arbor Michigan USA
| | - Brian A Larsen
- Los Alamos National Laboratory Los Alamos New Mexico USA
| | - Ruth M Skoug
- Los Alamos National Laboratory Los Alamos New Mexico USA
| | - Michael W Liemohn
- Department of Climate and Space Engineering University of Michigan Ann Arbor Michigan USA
| | - Aaron Breneman
- School of Physics and Astronomy University of Minnesota Minneapolis Minnesota USA
| | - John R Wygant
- School of Physics and Astronomy University of Minnesota Minneapolis Minnesota USA
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9
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Hartley DP, Chen Y, Kletzing CA, Denton MH, Kurth WS. Applying the cold plasma dispersion relation to whistler mode chorus waves: EMFISIS wave measurements from the Van Allen Probes. J Geophys Res Space Phys 2015; 120:1144-1152. [PMID: 26167444 PMCID: PMC4497456 DOI: 10.1002/2014ja020808] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/10/2014] [Accepted: 01/20/2015] [Indexed: 05/17/2023]
Abstract
Most theoretical wave models require the power in the wave magnetic field in order to determine the effect of chorus waves on radiation belt electrons. However, researchers typically use the cold plasma dispersion relation to approximate the magnetic wave power when only electric field data are available. In this study, the validity of using the cold plasma dispersion relation in this context is tested using Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) observations of both the electric and magnetic spectral intensities in the chorus wave band (0.1-0.9 fce). Results from this study indicate that the calculated wave intensity is least accurate during periods of enhanced wave activity. For observed wave intensities >10-3 nT2, using the cold plasma dispersion relation results in an underestimate of the wave intensity by a factor of 2 or greater 56% of the time over the full chorus wave band, 60% of the time for lower band chorus, and 59% of the time for upper band chorus. Hence, during active periods, empirical chorus wave models that are reliant on the cold plasma dispersion relation will underestimate chorus wave intensities to a significant degree, thus causing questionable calculation of wave-particle resonance effects on MeV electrons.
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Affiliation(s)
- D P Hartley
- Physics Department, Lancaster UniversityLancaster, UK
| | - Y Chen
- Los Alamos National LaboratoryLos Alamos, New Mexico, USA
| | - C A Kletzing
- Department of Physics and Astronomy, University of IowaIowa City, Iowa, USA
| | - M H Denton
- Space Science InstituteBoulder, Colorado, USA
| | - W S Kurth
- Department of Physics and Astronomy, University of IowaIowa City, Iowa, USA
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Li X, Selesnick RS, Baker DN, Jaynes AN, Kanekal SG, Schiller Q, Blum L, Fennell J, Blake JB. Upper limit on the inner radiation belt MeV electron intensity. J Geophys Res Space Phys 2015; 120:1215-1228. [PMID: 26167446 PMCID: PMC4497489 DOI: 10.1002/2014ja020777] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/29/2014] [Accepted: 01/14/2015] [Indexed: 06/01/2023]
Abstract
No instruments in the inner radiation belt are immune from the unforgiving penetration of the highly energetic protons (tens of MeV to GeV). The inner belt proton flux level, however, is relatively stable; thus, for any given instrument, the proton contamination often leads to a certain background noise. Measurements from the Relativistic Electron and Proton Telescope integrated little experiment on board Colorado Student Space Weather Experiment CubeSat, in a low Earth orbit, clearly demonstrate that there exist sub-MeV electrons in the inner belt because their flux level is orders of magnitude higher than the background, while higher-energy electron (>1.6 MeV) measurements cannot be distinguished from the background. Detailed analysis of high-quality measurements from the Relativistic Electron and Proton Telescope on board Van Allen Probes, in a geo-transfer-like orbit, provides, for the first time, quantified upper limits on MeV electron fluxes in various energy ranges in the inner belt. These upper limits are rather different from flux levels in the AE8 and AE9 models, which were developed based on older data sources. For 1.7, 2.5, and 3.3 MeV electrons, the upper limits are about 1 order of magnitude lower than predicted model fluxes. The implication of this difference is profound in that unless there are extreme solar wind conditions, which have not happened yet since the launch of Van Allen Probes, significant enhancements of MeV electrons do not occur in the inner belt even though such enhancements are commonly seen in the outer belt. KEY POINTS Quantified upper limit of MeV electrons in the inner beltActual MeV electron intensity likely much lower than the upper limitMore detailed understanding of relativistic electrons in the magnetosphere.
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Affiliation(s)
- X Li
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder Boulder, Colorado, USA ; Department of Aerospace Engineering Sciences, University of Colorado Boulder Boulder, Colorado, USA
| | - R S Selesnick
- Space Vehicles Directorate, Air Force Research Laboratory Kirtland AFB, New Mexico, USA
| | - D N Baker
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder Boulder, Colorado, USA
| | - A N Jaynes
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder Boulder, Colorado, USA
| | - S G Kanekal
- NASA/Goddard Space Flight Center Greenbelt, Maryland, USA
| | - Q Schiller
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder Boulder, Colorado, USA ; Department of Aerospace Engineering Sciences, University of Colorado Boulder Boulder, Colorado, USA
| | - L Blum
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder Boulder, Colorado, USA ; Department of Aerospace Engineering Sciences, University of Colorado Boulder Boulder, Colorado, USA ; Now at Space Sciences Laboratory, University of California Berkeley, California, USA
| | - J Fennell
- Space Science Applications Laboratory, Aerospace Corporation El Segundo, California, USA
| | - J B Blake
- Space Science Applications Laboratory, Aerospace Corporation El Segundo, California, USA
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Gerrard A, Lanzerotti L, Gkioulidou M, Mitchell D, Manweiler J, Bortnik J, Keika K. Initial measurements of O-ion and He-ion decay rates observed from the Van Allen probes RBSPICE instrument. J Geophys Res Space Phys 2014; 119:8813-8819. [PMID: 26167435 PMCID: PMC4497452 DOI: 10.1002/2014ja020374] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 07/07/2014] [Accepted: 10/06/2014] [Indexed: 06/04/2023]
Abstract
H-ion (∼45 keV to ∼600 keV), He-ion (∼65 keV to ∼520 keV), and O-ion (∼140 keV to ∼1130 keV) integral flux measurements, from the Radiation Belt Storm Probe Ion Composition Experiment (RBSPICE) instrument aboard the Van Allan Probes spacecraft B, are reported. These abundance data form a cohesive picture of ring current ions during the first 9 months of measurements. Furthermore, the data presented herein are used to show injection characteristics via the He-ion/H-ion abundance ratio and the O-ion/H-ion abundance ratio. Of unique interest to ring current dynamics are the spatial-temporal decay characteristics of the two injected populations. We observe that He-ions decay more quickly at lower L shells, on the order of ∼0.8 day at L shells of 3-4, and decay more slowly with higher L shell, on the order of ∼1.7 days at L shells of 5-6. Conversely, O-ions decay very rapidly (∼1.5 h) across all L shells. The He-ion decay time are consistent with previously measured and calculated lifetimes associated with charge exchange. The O-ion decay time is much faster than predicted and is attributed to the inclusion of higher-energy (> 500 keV) O-ions in our decay rate estimation. We note that these measurements demonstrate a compelling need for calculation of high-energy O-ion loss rates, which have not been adequately studied in the literature to date. KEY POINTS We report initial observations of ring current ionsWe show that He-ion decay rates are consistent with theoryWe show that O-ions with energies greater than 500 keV decay very rapidly.
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Affiliation(s)
- Andrew Gerrard
- Center for Solar-Terrestrial Research, New Jersey Institute of Technology Newark, New Jersey, USA
| | - Louis Lanzerotti
- Center for Solar-Terrestrial Research, New Jersey Institute of Technology Newark, New Jersey, USA
| | - Matina Gkioulidou
- John Hopkins University-Applied Physics Laboratory Laurel, Maryland, USA
| | - Donald Mitchell
- John Hopkins University-Applied Physics Laboratory Laurel, Maryland, USA
| | | | - Jacob Bortnik
- Department of Atmospheric and Oceanic Sciences, University of California Los Angeles, California, USA
| | - Kunihiro Keika
- Solar-Terrestrial Environment Laboratory, Nagoya University Nagoya, Japan
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Fu X, Cowee MM, Friedel RH, Funsten HO, Gary SP, Hospodarsky GB, Kletzing C, Kurth W, Larsen BA, Liu K, MacDonald EA, Min K, Reeves GD, Skoug RM, Winske D. Whistler anisotropy instabilities as the source of banded chorus: Van Allen Probes observations and particle-in-cell simulations. J Geophys Res Space Phys 2014; 119:8288-8298. [PMID: 26167433 PMCID: PMC4497467 DOI: 10.1002/2014ja020364] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/08/2014] [Accepted: 09/27/2014] [Indexed: 05/17/2023]
Abstract
Magnetospheric banded chorus is enhanced whistler waves with frequencies ωr <Ω e , where Ω e is the electron cyclotron frequency, and a characteristic spectral gap at ωr ≃Ω e /2. This paper uses spacecraft observations and two-dimensional particle-in-cell simulations in a magnetized, homogeneous, collisionless plasma to test the hypothesis that banded chorus is due to local linear growth of two branches of the whistler anisotropy instability excited by two distinct, anisotropic electron components of significantly different temperatures. The electron densities and temperatures are derived from Helium, Oxygen, Proton, and Electron instrument measurements on the Van Allen Probes A satellite during a banded chorus event on 1 November 2012. The observations are consistent with a three-component electron model consisting of a cold (a few tens of eV) population, a warm (a few hundred eV) anisotropic population, and a hot (a few keV) anisotropic population. The simulations use plasma and field parameters as measured from the satellite during this event except for two numbers: the anisotropies of the warm and the hot electron components are enhanced over the measured values in order to obtain relatively rapid instability growth. The simulations show that the warm component drives the quasi-electrostatic upper band chorus and that the hot component drives the electromagnetic lower band chorus; the gap at ∼Ω e /2 is a natural consequence of the growth of two whistler modes with different properties.
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Affiliation(s)
- Xiangrong Fu
- Los Alamos National LaboratoryLos Alamos, New Mexico, USA
| | - Misa M Cowee
- Los Alamos National LaboratoryLos Alamos, New Mexico, USA
| | | | | | | | | | - Craig Kletzing
- Department of Physics and Astronomy, University of IowaIowa City, Iowa, USA
| | - William Kurth
- Department of Physics and Astronomy, University of IowaIowa City, Iowa, USA
| | - Brian A Larsen
- Los Alamos National LaboratoryLos Alamos, New Mexico, USA
| | - Kaijun Liu
- Department of Physics, Auburn UniversityAuburn, Alabama, USA
| | | | - Kyungguk Min
- Department of Physics, Auburn UniversityAuburn, Alabama, USA
| | | | - Ruth M Skoug
- Los Alamos National LaboratoryLos Alamos, New Mexico, USA
| | - Dan Winske
- Los Alamos National LaboratoryLos Alamos, New Mexico, USA
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