1
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Phan TD, Verniero JL, Larson D, Lavraud B, Drake JF, Øieroset M, Eastwood JP, Bale SD, Livi R, Halekas JS, Whittlesey PL, Rahmati A, Stansby D, Pulupa M, MacDowall RJ, Szabo PA, Koval A, Desai M, Fuselier SA, Velli M, Hesse M, Pyakurel PS, Maheshwari K, Kasper JC, Stevens JM, Case AW, Raouafi NE. Parker Solar Probe Observations of Solar Wind Energetic Proton Beams Produced by Magnetic Reconnection in the Near-Sun Heliospheric Current Sheet. Geophys Res Lett 2022; 49:e2021GL096986. [PMID: 35864893 PMCID: PMC9286436 DOI: 10.1029/2021gl096986] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/09/2021] [Revised: 03/21/2022] [Accepted: 03/30/2022] [Indexed: 06/09/2023]
Abstract
We report observations of reconnection exhausts in the Heliospheric Current Sheet (HCS) during Parker Solar Probe Encounters 08 and 07, at 16 R s and 20 R s , respectively. Heliospheric current sheet (HCS) reconnection accelerated protons to almost twice the solar wind speed and increased the proton core energy by a factor of ∼3, due to the Alfvén speed being comparable to the solar wind flow speed at these near-Sun distances. Furthermore, protons were energized to super-thermal energies. During E08, energized protons were found to have leaked out of the exhaust along separatrix field lines, appearing as field-aligned energetic proton beams in a broad region outside the HCS. Concurrent dropouts of strahl electrons, indicating disconnection from the Sun, provide further evidence for the HCS being the source of the beams. Around the HCS in E07, there were also proton beams but without electron strahl dropouts, indicating that their origin was not the local HCS reconnection exhaust.
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Affiliation(s)
- T. D. Phan
- SSLUniversity of CaliforniaBerkeleyCAUSA
| | | | - D. Larson
- SSLUniversity of CaliforniaBerkeleyCAUSA
| | - B. Lavraud
- Laboratoire d'Astrophysique de BordeauxUniversity BordeauxPessacFrance
- IRAPCNRSCNESUniversité de ToulouseToulouseFrance
| | | | | | | | - S. D. Bale
- SSLUniversity of CaliforniaBerkeleyCAUSA
- Physics DepartmentUniversity of CaliforniaBerkeleyCAUSA
| | - R. Livi
- SSLUniversity of CaliforniaBerkeleyCAUSA
| | | | | | - A. Rahmati
- SSLUniversity of CaliforniaBerkeleyCAUSA
| | - D. Stansby
- Mullard Space Science LaboratoryUniversity College LondonDorkingUK
| | - M. Pulupa
- SSLUniversity of CaliforniaBerkeleyCAUSA
| | | | - P. A. Szabo
- NASA Goddard Space Flight CenterGreenbeltMDUSA
| | - A. Koval
- NASA Goddard Space Flight CenterGreenbeltMDUSA
- University of MarylandBaltimore CountyBaltimoreMDUSA
| | - M. Desai
- Southwest Research InstituteSan AntonioTXUSA
| | | | - M. Velli
- University of CaliforniaLos AngelesCAUSA
| | - M. Hesse
- NASA Ames Research CenterMoffett FieldCAUSA
| | | | | | - J. C. Kasper
- Climate and Space Sciences and EngineeringUniversity of MichiganAnn ArborMIUSA
| | | | - A. W. Case
- Smithsonian Astrophysical ObservatoryCambridgeMAUSA
| | - N. E. Raouafi
- Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
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2
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Malaspina DM, Goodrich K, Livi R, Halekas J, McManus M, Curry S, Bale SD, Bonnell JW, de Wit TD, Goetz K, Harvey PR, MacDowall RJ, Pulupa M, Case AW, Kasper JC, Korreck KE, Larson D, Stevens ML, Whittlesey P. Plasma Double Layers at the Boundary Between Venus and the Solar Wind. Geophys Res Lett 2020; 47:e2020GL090115. [PMID: 33380758 PMCID: PMC7757269 DOI: 10.1029/2020gl090115] [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] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 07/30/2020] [Revised: 09/14/2020] [Accepted: 10/03/2020] [Indexed: 06/12/2023]
Abstract
The solar wind is slowed, deflected, and heated as it encounters Venus's induced magnetosphere. The importance of kinetic plasma processes to these interactions has not been examined in detail, due to a lack of constraining observations. In this study, kinetic-scale electric field structures are identified in the Venusian magnetosheath, including plasma double layers. The double layers may be driven by currents or mixing of inhomogeneous plasmas near the edge of the magnetosheath. Estimated double-layer spatial scales are consistent with those reported at Earth. Estimated potential drops are similar to electron temperature gradients across the bow shock. Many double layers are found in few high cadence data captures, suggesting that their amplitudes are high relative to other magnetosheath plasma waves. These are the first direct observations of plasma double layers beyond near-Earth space, supporting the idea that kinetic plasma processes are active in many space plasma environments.
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Affiliation(s)
- D. M. Malaspina
- Department of Astrophysical and Planetary SciencesUniversity of Colorado BoulderBoulderCOUSA
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
| | - K. Goodrich
- Space Sciences LaboratoryUniversity of CaliforniaBerkeleyCAUSA
| | - R. Livi
- Space Sciences LaboratoryUniversity of CaliforniaBerkeleyCAUSA
| | - J. Halekas
- Department of Physics and AstronomyUniversity of IowaIowa CityIAUSA
| | - M. McManus
- Space Sciences LaboratoryUniversity of CaliforniaBerkeleyCAUSA
| | - S. Curry
- Space Sciences LaboratoryUniversity of CaliforniaBerkeleyCAUSA
| | - S. D. Bale
- Space Sciences LaboratoryUniversity of CaliforniaBerkeleyCAUSA
- Physics DepartmentUniversity of CaliforniaBerkeleyCAUSA
| | - J. W. Bonnell
- Space Sciences LaboratoryUniversity of CaliforniaBerkeleyCAUSA
| | | | - K. Goetz
- School of Physics and AstronomyUniversity of Minnesota, Twin CitiesMinneapolisMNUSA
| | - P. R. Harvey
- Space Sciences LaboratoryUniversity of CaliforniaBerkeleyCAUSA
| | | | - M. Pulupa
- Space Sciences LaboratoryUniversity of CaliforniaBerkeleyCAUSA
| | - A. W. Case
- Harvard‐Smithsonian Center for AstrophysicsCambridgeMAUSA
| | - J. C. Kasper
- Climate and Space Sciences and EngineeringUniversity of MichiganAnn ArborMIUSA
| | - K. E. Korreck
- Harvard‐Smithsonian Center for AstrophysicsCambridgeMAUSA
| | - D. Larson
- Space Sciences LaboratoryUniversity of CaliforniaBerkeleyCAUSA
| | - M. L. Stevens
- Harvard‐Smithsonian Center for AstrophysicsCambridgeMAUSA
| | - P. Whittlesey
- Space Sciences LaboratoryUniversity of CaliforniaBerkeleyCAUSA
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3
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Nosé M, Matsuoka A, Kumamoto A, Kasahara Y, Teramoto M, Kurita S, Goldstein J, Kistler LM, Singh S, Gololobov A, Shiokawa K, Imajo S, Oimatsu S, Yamamoto K, Obana Y, Shoji M, Tsuchiya F, Shinohara I, Miyoshi Y, Kurth WS, Kletzing CA, Smith CW, MacDowall RJ, Spence H, Reeves GD. Oxygen torus and its coincidence with EMIC wave in the deep inner magnetosphere: Van Allen Probe B and Arase observations. Earth Planets Space 2020; 72:111. [PMID: 32831576 PMCID: PMC7410109 DOI: 10.1186/s40623-020-01235-w] [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: 02/22/2020] [Accepted: 07/17/2020] [Indexed: 06/11/2023]
Abstract
We investigate the longitudinal structure of the oxygen torus in the inner magnetosphere for a specific event found on 12 September 2017, using simultaneous observations from the Van Allen Probe B and Arase satellites. It is found that Probe B observed a clear enhancement in the average plasma mass (M) up to 3-4 amu at L = 3.3-3.6 and magnetic local time (MLT) = 9.0 h. In the afternoon sector at MLT ~ 16.0 h, both Probe B and Arase found no clear enhancements in M. This result suggests that the oxygen torus does not extend over all MLT but is skewed toward the dawn. Since a similar result has been reported for another event of the oxygen torus in a previous study, a crescent-shaped torus or a pinched torus centered around dawn may be a general feature of the O+ density enhancement in the inner magnetosphere. We newly find that an electromagnetic ion cyclotron (EMIC) wave in the H+ band appeared coincidently with the oxygen torus. From the lower cutoff frequency of the EMIC wave, the ion composition of the oxygen torus is estimated to be 80.6% H+, 3.4% He+, and 16.0% O+. According to the linearized dispersion relation for EMIC waves, both He+ and O+ ions inhibit EMIC wave growth and the stabilizing effect is stronger for He+ than O+. Therefore, when the H+ fraction or M is constant, the denser O+ ions are naturally accompanied by the more tenuous He+ ions, resulting in a weaker stabilizing effect (i.e., larger growth rate). From the Probe B observations, we find that the growth rate becomes larger in the oxygen torus than in the adjacent regions in the plasma trough and the plasmasphere.
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Affiliation(s)
- M. Nosé
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Japan
| | - A. Matsuoka
- Graduate School of Science, Kyoto University, Kyoto, Japan
| | - A. Kumamoto
- Graduate School of Science, Tohoku University, Sendai, Japan
| | - Y. Kasahara
- Advanced Research Center for Space Science and Technology, Kanazawa University, Kanazawa, Japan
| | - M. Teramoto
- Department of Space Systems Engineering, Kyushu Institute of Technology, Kitakyusyu, Japan
| | - S. Kurita
- Research Institute for Sustainable Humanosphere, Kyoto University, Uji, Japan
| | - J. Goldstein
- Space Science and Engineering Division, Southwest Research Institute, San Antonio, TX USA
- University of Texas at San Antonio, San Antonio, TX USA
| | - L. M. Kistler
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Japan
- Institute for the Study of Earth, Oceans, and Space, University of New Hampshire, Durham, NH USA
| | - S. Singh
- Indian Institute of Geomagnetism, Navi Mumbai, India
| | - A. Gololobov
- North-Eastern Federal University, Yakutsk, Russia
| | - K. Shiokawa
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Japan
| | - S. Imajo
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Japan
| | - S. Oimatsu
- Graduate School of Science, Kyoto University, Kyoto, Japan
| | - K. Yamamoto
- Graduate School of Science, The University of Tokyo, Tokyo, Japan
| | - Y. Obana
- Faculty of Engineering, Osaka Electro-Communication University, Neyagawa, Japan
| | - M. Shoji
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Japan
| | - F. Tsuchiya
- Graduate School of Science, Tohoku University, Sendai, Japan
| | - I. Shinohara
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - Y. Miyoshi
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Japan
| | - W. S. Kurth
- Department of Physics and Astronomy, University of Iowa, Iowa City, IA USA
| | - C. A. Kletzing
- Department of Physics and Astronomy, University of Iowa, Iowa City, IA USA
| | - C. W. Smith
- Institute for the Study of Earth, Oceans, and Space, University of New Hampshire, Durham, NH USA
| | - R. J. MacDowall
- Solar System Exploration Division, Goddard Space Flight Center, Greenbelt, MD USA
| | - H. Spence
- Institute for the Study of Earth, Oceans, and Space, University of New Hampshire, Durham, NH USA
| | - G. D. Reeves
- Space Sciences and Applications Group, Los Alamos National Laboratory, Los Alamos, NM USA
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4
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Kasper JC, Bale SD, Belcher JW, Berthomier M, Case AW, Chandran BDG, Curtis DW, Gallagher D, Gary SP, Golub L, Halekas JS, Ho GC, Horbury TS, Hu Q, Huang J, Klein KG, Korreck KE, Larson DE, Livi R, Maruca B, Lavraud B, Louarn P, Maksimovic M, Martinovic M, McGinnis D, Pogorelov NV, Richardson JD, Skoug RM, Steinberg JT, Stevens ML, Szabo A, Velli M, Whittlesey PL, Wright KH, Zank GP, MacDowall RJ, McComas DJ, McNutt RL, Pulupa M, Raouafi NE, Schwadron NA. Alfvénic velocity spikes and rotational flows in the near-Sun solar wind. Nature 2019; 576:228-231. [PMID: 31802006 DOI: 10.1038/s41586-019-1813-z] [Citation(s) in RCA: 216] [Impact Index Per Article: 43.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/18/2019] [Accepted: 10/17/2019] [Indexed: 11/09/2022]
Abstract
The prediction of a supersonic solar wind1 was first confirmed by spacecraft near Earth2,3 and later by spacecraft at heliocentric distances as small as 62 solar radii4. These missions showed that plasma accelerates as it emerges from the corona, aided by unidentified processes that transport energy outwards from the Sun before depositing it in the wind. Alfvénic fluctuations are a promising candidate for such a process because they are seen in the corona and solar wind and contain considerable energy5-7. Magnetic tension forces the corona to co-rotate with the Sun, but any residual rotation far from the Sun reported until now has been much smaller than the amplitude of waves and deflections from interacting wind streams8. Here we report observations of solar-wind plasma at heliocentric distances of about 35 solar radii9-11, well within the distance at which stream interactions become important. We find that Alfvén waves organize into structured velocity spikes with duration of up to minutes, which are associated with propagating S-like bends in the magnetic-field lines. We detect an increasing rotational component to the flow velocity of the solar wind around the Sun, peaking at 35 to 50 kilometres per second-considerably above the amplitude of the waves. These flows exceed classical velocity predictions of a few kilometres per second, challenging models of circulation in the corona and calling into question our understanding of how stars lose angular momentum and spin down as they age12-14.
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Affiliation(s)
- J C Kasper
- Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA. .,Smithsonian Astrophysical Observatory, Cambridge, MA, USA.
| | - S D Bale
- Physics Department, University of California, Berkeley, CA, USA.,Space Sciences Laboratory, University of California, Berkeley, CA, USA.,The Blackett Laboratory, Imperial College London, London, UK
| | - J W Belcher
- Kavli Center for Astrophysics and Space Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - M Berthomier
- Laboratoire de Physique des Plasmas, CNRS, Sorbonne Université, Ecole Polytechnique, Observatoire de Paris, Université Paris-Saclay, Paris, France
| | - A W Case
- Smithsonian Astrophysical Observatory, Cambridge, MA, USA
| | - B D G Chandran
- Department of Physics and Astronomy, University of New Hampshire, Durham, NH, USA.,Space Science Center, University of New Hampshire, Durham, NH, USA
| | - D W Curtis
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - D Gallagher
- Heliophysics and Planetary Science Branch ST13, Marshall Space Flight Center, Huntsville, AL, USA
| | - S P Gary
- Los Alamos National Laboratory, Los Alamos, NM, USA
| | - L Golub
- Smithsonian Astrophysical Observatory, Cambridge, MA, USA
| | - J S Halekas
- Department of Physics and Astronomy, University of Iowa, IA, USA
| | - G C Ho
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - T S Horbury
- The Blackett Laboratory, Imperial College London, London, UK
| | - Q Hu
- Department of Space Science and Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, Huntsville, AL, USA
| | - J Huang
- Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA
| | - K G Klein
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA.,Department of Planetary Sciences, University of Arizona, Tucson, AZ, USA
| | - K E Korreck
- Smithsonian Astrophysical Observatory, Cambridge, MA, USA
| | - D E Larson
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - R Livi
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - B Maruca
- Department of Physics and Astronomy, University of Delaware, Newark, DE, USA.,Bartol Research Institute, University of Delaware, Newark, DE, USA
| | - B Lavraud
- Institut de Recherche en Astrophysique et Planétologie, CNRS, UPS, CNES, Université de Toulouse, Toulouse, France
| | - P Louarn
- Institut de Recherche en Astrophysique et Planétologie, CNRS, UPS, CNES, Université de Toulouse, Toulouse, France
| | - M Maksimovic
- LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, Meudon, France
| | - M Martinovic
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | - D McGinnis
- Department of Physics and Astronomy, University of Iowa, IA, USA
| | - N V Pogorelov
- Department of Space Science and Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, Huntsville, AL, USA
| | - J D Richardson
- Kavli Center for Astrophysics and Space Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - R M Skoug
- Los Alamos National Laboratory, Los Alamos, NM, USA
| | | | - M L Stevens
- Smithsonian Astrophysical Observatory, Cambridge, MA, USA
| | - A Szabo
- NASA/Goddard Space Flight Center, Greenbelt, MD, USA
| | - M Velli
- Department of Earth, Planetary and Space Sciences, University of California, Los Angeles, CA, USA
| | - P L Whittlesey
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - K H Wright
- Universities Space Research Association, Science and Technology Institute, Huntsville, AL, USA
| | - G P Zank
- Department of Space Science and Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, Huntsville, AL, USA
| | - R J MacDowall
- NASA/Goddard Space Flight Center, Greenbelt, MD, USA
| | - D J McComas
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA
| | - R L McNutt
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - M Pulupa
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - N E Raouafi
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - N A Schwadron
- Department of Physics and Astronomy, University of New Hampshire, Durham, NH, USA.,Space Science Center, University of New Hampshire, Durham, NH, USA
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5
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McComas DJ, Christian ER, Cohen CMS, Cummings AC, Davis AJ, Desai MI, Giacalone J, Hill ME, Joyce CJ, Krimigis SM, Labrador AW, Leske RA, Malandraki O, Matthaeus WH, McNutt RL, Mewaldt RA, Mitchell DG, Posner A, Rankin JS, Roelof EC, Schwadron NA, Stone EC, Szalay JR, Wiedenbeck ME, Bale SD, Kasper JC, Case AW, Korreck KE, MacDowall RJ, Pulupa M, Stevens ML, Rouillard AP. Probing the energetic particle environment near the Sun. Nature 2019; 576:223-227. [PMID: 31802005 PMCID: PMC6908744 DOI: 10.1038/s41586-019-1811-1] [Citation(s) in RCA: 77] [Impact Index Per Article: 15.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/28/2019] [Accepted: 09/05/2019] [Indexed: 11/18/2022]
Abstract
NASA's Parker Solar Probe mission1 recently plunged through the inner heliosphere of the Sun to its perihelia, about 24 million kilometres from the Sun. Previous studies farther from the Sun (performed mostly at a distance of 1 astronomical unit) indicate that solar energetic particles are accelerated from a few kiloelectronvolts up to near-relativistic energies via at least two processes: 'impulsive' events, which are usually associated with magnetic reconnection in solar flares and are typically enriched in electrons, helium-3 and heavier ions2, and 'gradual' events3,4, which are typically associated with large coronal-mass-ejection-driven shocks and compressions moving through the corona and inner solar wind and are the dominant source of protons with energies between 1 and 10 megaelectronvolts. However, some events show aspects of both processes and the electron-proton ratio is not bimodally distributed, as would be expected if there were only two possible processes5. These processes have been very difficult to resolve from prior observations, owing to the various transport effects that affect the energetic particle population en route to more distant spacecraft6. Here we report observations of the near-Sun energetic particle radiation environment over the first two orbits of the probe. We find a variety of energetic particle events accelerated both locally and remotely including by corotating interaction regions, impulsive events driven by acceleration near the Sun, and an event related to a coronal mass ejection. We provide direct observations of the energetic particle radiation environment in the region just above the corona of the Sun and directly explore the physics of particle acceleration and transport.
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Affiliation(s)
- D J McComas
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA.
| | | | - C M S Cohen
- California Institute of Technology, Pasadena, CA, USA
| | - A C Cummings
- California Institute of Technology, Pasadena, CA, USA
| | - A J Davis
- California Institute of Technology, Pasadena, CA, USA
| | - M I Desai
- Southwest Research Institute, San Antonio, TX, USA
- University of Texas at San Antonio, San Antonio, TX, USA
| | | | - M E Hill
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - C J Joyce
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA
| | - S M Krimigis
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - A W Labrador
- California Institute of Technology, Pasadena, CA, USA
| | - R A Leske
- California Institute of Technology, Pasadena, CA, USA
| | - O Malandraki
- National Observatory of Athens, IAASARS, Athens, Greece
| | | | - R L McNutt
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - R A Mewaldt
- California Institute of Technology, Pasadena, CA, USA
| | - D G Mitchell
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | | | - J S Rankin
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA
| | - E C Roelof
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - N A Schwadron
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA
- University of New Hampshire, Durham, NH, USA
| | - E C Stone
- California Institute of Technology, Pasadena, CA, USA
| | - J R Szalay
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA
| | - M E Wiedenbeck
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - S D Bale
- University of California at Berkeley, Berkeley, CA, USA
- The Blackett Laboratory, Imperial College London, London, UK
| | - J C Kasper
- University of Michigan, Ann Arbor, MI, USA
| | - A W Case
- Smithsonian Astrophysical Observatory, Cambridge, MA, USA
| | - K E Korreck
- Smithsonian Astrophysical Observatory, Cambridge, MA, USA
| | | | - M Pulupa
- University of California at Berkeley, Berkeley, CA, USA
| | - M L Stevens
- Smithsonian Astrophysical Observatory, Cambridge, MA, USA
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6
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Farrell WM, Wahlund JE, Morooka M, Kurth WS, Gurnett DA, MacDowall RJ. Ion Trapping by Dust Grains: Simulation Applications to the Enceladus Plume. J Geophys Res Planets 2017; 122:729-743. [PMID: 32021741 PMCID: PMC6999740 DOI: 10.1002/2016je005235] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
Using a particle-in-cell electrostatic simulation, we examine the conditions that allow low energy ions, like those produced in the Enceladus plume, to be attracted and trapped within the sheaths of negatively-charged dust grains. The conventional wisdom is that all new ions produced in the Enceladus plume are free to get picked up (i.e., accelerated by the local E-field to then undergo vB acceleration). However, we suggest herein that the presence of submicron charged dust in the plume impedes this pickup process since the local grain electric field greatly exceeds the co-rotation E-fields. The simulations demonstrate that cold ions will tend to accelerate toward the negatively charged grains and become part of the ion plasma sheath. These trapped ions will move with the grains, exiting the plume region at the dust speed. We suggest that Cassini's Langmuir probe is measuring the entire ion population (free and trapped ions), while the Cassini magnetometer detects the magnetic perturbations associated with pickup currents from the smaller population of free ions, with this distinction possibly reconciling the ongoing debate in the literature on the ion density in the plume.
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Affiliation(s)
- W M Farrell
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - J-E Wahlund
- Swedish Institute of Space Physics, Uppsala, Sweden
| | - M Morooka
- Swedish Institute of Space Physics, Uppsala, Sweden
| | - W S Kurth
- University of Iowa, Iowa City, IA, USA
| | | | - R J MacDowall
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
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7
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Thejappa G, MacDowall RJ. Critical Fluctuations in Beam-Plasma Systems and Solar Type III Radio Bursts. J Phys Conf Ser 2017; 900:012019. [PMID: 33510810 PMCID: PMC7839983 DOI: 10.1088/1742-6596/900/1/012019] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
It is shown that the Langmuir waves are excited similar to critical fluctuations during phase transitions when the negative absorption due to electron beam traveling radially outward in the solar atmosphere is balanced by the positive absorption due to collisions in the corona and due to scattering on electron density inhomogeneities in the interplanetary medium. The effective temperature of the Langmuir fluctuations range from 1011 to 1013 K, explaining the majority of the type III bursts. The Rayleigh scattering and direct coupling due to density gradient as well as due to density inhomogeneities are discussed in the context of fundamental radiation and the combination scattering for second harmonic. The number density of electrons in type III beams is estimated and compared with observations. It is also shown that the stabilization of type III beams is achieved automatically since the instability does not develop in the case of critical fluctuations.
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Affiliation(s)
- G Thejappa
- Department of Astronomy, University of Maryland, College Park, MD 20742, USA
| | - R J MacDowall
- NASA/Goddard Space Flight Center, Greenbelt MD 20771, USA
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8
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Bale SD, Goetz K, Harvey PR, Turin P, Bonnell JW, de Wit TD, Ergun RE, MacDowall RJ, Pulupa M, Andre M, Bolton M, Bougeret JL, Bowen TA, Burgess D, Cattell CA, Chandran BDG, Chaston CC, Chen CHK, Choi MK, Connerney JE, Cranmer S, Diaz-Aguado M, Donakowski W, Drake JF, Farrell WM, Fergeau P, Fermin J, Fischer J, Fox N, Glaser D, Goldstein M, Gordon D, Hanson E, Harris SE, Hayes LM, Hinze JJ, Hollweg JV, Horbury TS, Howard RA, Hoxie V, Jannet G, Karlsson M, Kasper JC, Kellogg PJ, Kien M, Klimchuk JA, Krasnoselskikh VV, Krucker S, Lynch JJ, Maksimovic M, Malaspina DM, Marker S, Martin P, Martinez-Oliveros J, McCauley J, McComas DJ, McDonald T, Meyer-Vernet N, Moncuquet M, Monson SJ, Mozer FS, Murphy SD, Odom J, Oliverson R, Olson J, Parker EN, Pankow D, Phan T, Quataert E, Quinn T, Ruplin SW, Salem C, Seitz D, Sheppard DA, Siy A, Stevens K, Summers D, Szabo A, Timofeeva M, Vaivads A, Velli M, Yehle A, Werthimer D, Wygant JR. The FIELDS Instrument Suite for Solar Probe Plus: Measuring the Coronal Plasma and Magnetic Field, Plasma Waves and Turbulence, and Radio Signatures of Solar Transients. Space Sci Rev 2016; 204:49-82. [PMID: 29755144 PMCID: PMC5942226 DOI: 10.1007/s11214-016-0244-5] [Citation(s) in RCA: 10] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/31/2023]
Abstract
NASA's Solar Probe Plus (SPP) mission will make the first in situ measurements of the solar corona and the birthplace of the solar wind. The FIELDS instrument suite on SPP will make direct measurements of electric and magnetic fields, the properties of in situ plasma waves, electron density and temperature profiles, and interplanetary radio emissions, amongst other things. Here, we describe the scientific objectives targeted by the SPP/FIELDS instrument, the instrument design itself, and the instrument concept of operations and planned data products.
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Affiliation(s)
- S D Bale
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
- Physics Department, University of California, Berkeley, CA, USA
| | - K Goetz
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA
| | - P R Harvey
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - P Turin
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - J W Bonnell
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - T Dudok de Wit
- LPC2E, CNRS, 3A avenue de la Recherche Scientifique, Orléans, France
| | - R E Ergun
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA
| | - R J MacDowall
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - M Pulupa
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - M Andre
- Swedish Institute of Space Physics (IRF), Uppsala, Sweden
| | - M Bolton
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA
| | | | - T A Bowen
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
- Physics Department, University of California, Berkeley, CA, USA
| | - D Burgess
- Astronomy Unit, Queen Mary, University of London, London, UK
| | - C A Cattell
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA
| | - B D G Chandran
- Department of Physics, University of New Hampshire, Durham, NH, USA
| | - C C Chaston
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - C H K Chen
- Department of Physics, Imperial College, London, UK
| | - M K Choi
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - J E Connerney
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - S Cranmer
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA
| | - M Diaz-Aguado
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - W Donakowski
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - J F Drake
- Department of Physics, University of Maryland, College Park, MD, USA
| | - W M Farrell
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - P Fergeau
- LPC2E, CNRS, 3A avenue de la Recherche Scientifique, Orléans, France
| | - J Fermin
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - J Fischer
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - N Fox
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - D Glaser
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - M Goldstein
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - D Gordon
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - E Hanson
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
- Physics Department, University of California, Berkeley, CA, USA
| | - S E Harris
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - L M Hayes
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - J J Hinze
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA
| | - J V Hollweg
- Department of Physics, University of New Hampshire, Durham, NH, USA
| | - T S Horbury
- Department of Physics, Imperial College, London, UK
| | - R A Howard
- Space Science Division, Naval Research Laboratory, Washington, DC, USA
| | - V Hoxie
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA
| | - G Jannet
- LPC2E, CNRS, 3A avenue de la Recherche Scientifique, Orléans, France
| | - M Karlsson
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA
| | - J C Kasper
- University of Michigan, Ann Arbor, MI, USA
| | - P J Kellogg
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA
| | - M Kien
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA
| | - J A Klimchuk
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | | | - S Krucker
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - J J Lynch
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA
| | | | - D M Malaspina
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA
| | - S Marker
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - P Martin
- LPC2E, CNRS, 3A avenue de la Recherche Scientifique, Orléans, France
| | | | - J McCauley
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - D J McComas
- Southwest Research Institute, San Antonio, TX, USA
| | - T McDonald
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | | | - M Moncuquet
- LESIA, Observatoire de Paris, Meudon, France
| | - S J Monson
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA
| | - F S Mozer
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - S D Murphy
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - J Odom
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - R Oliverson
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - J Olson
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - E N Parker
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA
| | - D Pankow
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - T Phan
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - E Quataert
- Astronomy Department, University of California, Berkeley, CA, USA
| | - T Quinn
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | | | - C Salem
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - D Seitz
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - D A Sheppard
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - A Siy
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - K Stevens
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA
| | - D Summers
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA
| | - A Szabo
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - M Timofeeva
- LPC2E, CNRS, 3A avenue de la Recherche Scientifique, Orléans, France
| | - A Vaivads
- Swedish Institute of Space Physics (IRF), Uppsala, Sweden
| | - M Velli
- Earth, Planetary, and Space Sciences, UCLA, Los Angelos, CA, USA
| | - A Yehle
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA
| | - D Werthimer
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | - J R Wygant
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA
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McComas DJ, Allegrini F, Bochsler P, Bzowski M, Christian ER, Crew GB, DeMajistre R, Fahr H, Fichtner H, Frisch PC, Funsten HO, Fuselier SA, Gloeckler G, Gruntman M, Heerikhuisen J, Izmodenov V, Janzen P, Knappenberger P, Krimigis S, Kucharek H, Lee M, Livadiotis G, Livi S, MacDowall RJ, Mitchell D, Möbius E, Moore T, Pogorelov NV, Reisenfeld D, Roelof E, Saul L, Schwadron NA, Valek PW, Vanderspek R, Wurz P, Zank GP. Global observations of the interstellar interaction from the Interstellar Boundary Explorer (IBEX). Science 2009; 326:959-962. [PMID: 19833923 DOI: 10.1007/s11214-009-9499-4] [Citation(s) in RCA: 23] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/17/2008] [Accepted: 03/23/2009] [Indexed: 05/23/2023]
Abstract
The Sun moves through the local interstellar medium, continuously emitting ionized, supersonic solar wind plasma and carving out a cavity in interstellar space called the heliosphere. The recently launched Interstellar Boundary Explorer (IBEX) spacecraft has completed its first all-sky maps of the interstellar interaction at the edge of the heliosphere by imaging energetic neutral atoms (ENAs) emanating from this region. We found a bright ribbon of ENA emission, unpredicted by prior models or theories, that may be ordered by the local interstellar magnetic field interacting with the heliosphere. This ribbon is superposed on globally distributed flux variations ordered by both the solar wind structure and the direction of motion through the interstellar medium. Our results indicate that the external galactic environment strongly imprints the heliosphere.
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Affiliation(s)
- D J McComas
- Southwest Research Institute, San Antonio, TX 78228, USA.
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10
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McComas DJ, Allegrini F, Bochsler P, Bzowski M, Christian ER, Crew GB, DeMajistre R, Fahr H, Fichtner H, Frisch PC, Funsten HO, Fuselier SA, Gloeckler G, Gruntman M, Heerikhuisen J, Izmodenov V, Janzen P, Knappenberger P, Krimigis S, Kucharek H, Lee M, Livadiotis G, Livi S, MacDowall RJ, Mitchell D, Möbius E, Moore T, Pogorelov NV, Reisenfeld D, Roelof E, Saul L, Schwadron NA, Valek PW, Vanderspek R, Wurz P, Zank GP. Global observations of the interstellar interaction from the Interstellar Boundary Explorer (IBEX). Science 2009; 326:959-62. [PMID: 19833923 DOI: 10.1126/science.1180906] [Citation(s) in RCA: 390] [Impact Index Per Article: 26.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Sun moves through the local interstellar medium, continuously emitting ionized, supersonic solar wind plasma and carving out a cavity in interstellar space called the heliosphere. The recently launched Interstellar Boundary Explorer (IBEX) spacecraft has completed its first all-sky maps of the interstellar interaction at the edge of the heliosphere by imaging energetic neutral atoms (ENAs) emanating from this region. We found a bright ribbon of ENA emission, unpredicted by prior models or theories, that may be ordered by the local interstellar magnetic field interacting with the heliosphere. This ribbon is superposed on globally distributed flux variations ordered by both the solar wind structure and the direction of motion through the interstellar medium. Our results indicate that the external galactic environment strongly imprints the heliosphere.
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Affiliation(s)
- D J McComas
- Southwest Research Institute, San Antonio, TX 78228, USA.
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11
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Smith EJ, Marsden RG, Balogh A, Gloeckler G, Geiss J, McComas DJ, McKibben RB, MacDowall RJ, Lanzerotti LJ, Krupp N, Krueger H, Landgraf M. The Sun and Heliosphere at Solar Maximum. Science 2003; 302:1165-9. [PMID: 14615526 DOI: 10.1126/science.1086295] [Citation(s) in RCA: 51] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Recent Ulysses observations from the Sun's equator to the poles reveal fundamental properties of the three-dimensional heliosphere at the maximum in solar activity. The heliospheric magnetic field originates from a magnetic dipole oriented nearly perpendicular to, instead of nearly parallel to, the Sun's rotation axis. Magnetic fields, solar wind, and energetic charged particles from low-latitude sources reach all latitudes, including the polar caps. The very fast high-latitude wind and polar coronal holes disappear and reappear together. Solar wind speed continues to be inversely correlated with coronal temperature. The cosmic ray flux is reduced symmetrically at all latitudes.
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Affiliation(s)
- E J Smith
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
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Thejappa G, Goldstein ML, MacDowall RJ, Papadopoulos K, Stone RG. Evidence for Langmuir envelope solitons in solar type III burst source regions. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/1999ja900363] [Citation(s) in RCA: 28] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Lin N, Kellogg PJ, MacDowall RJ, Mei Y, Cornilleau-Wehrlin N, Canu P, de Villedary C, Rezeau L, Balogh A, Forsyth RJ. ULF Waves in the Io Torus: Ulysses Observations. ACTA ACUST UNITED AC 1993. [DOI: 10.1029/93ja02593] [Citation(s) in RCA: 16] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Farrell WM, MacDowall RJ, Hess RA, Kaiser ML, Desch MD, Stone RG. An Interpretation of the Broadband VLF Waves Near the Io Torus as Observed by Ulysses. ACTA ACUST UNITED AC 1993. [DOI: 10.1029/93ja02591] [Citation(s) in RCA: 16] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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