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1
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Bowen TA, Mallet A, Bale SD, Bonnell JW, Case AW, Chandran BDG, Chasapis A, Chen CHK, Duan D, Dudok de Wit T, Goetz K, Halekas JS, Harvey PR, Kasper JC, Korreck KE, Larson D, Livi R, MacDowall RJ, Malaspina DM, McManus MD, Pulupa M, Stevens M, Whittlesey P. Constraining Ion-Scale Heating and Spectral Energy Transfer in Observations of Plasma Turbulence. Phys Rev Lett 2020; 125:025102. [PMID: 32701332 DOI: 10.1103/physrevlett.125.025102] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/14/2020] [Revised: 05/11/2020] [Accepted: 05/22/2020] [Indexed: 06/11/2023]
Abstract
We perform a statistical study of the turbulent power spectrum at inertial and kinetic scales observed during the first perihelion encounter of the Parker Solar Probe. We find that often there is an extremely steep scaling range of the power spectrum just above the ion-kinetic scales, similar to prior observations at 1 A.U., with a power-law index of around -4. Based on our measurements, we demonstrate that either a significant (>50%) fraction of the total turbulent energy flux is dissipated in this range of scales, or the characteristic nonlinear interaction time of the turbulence decreases dramatically from the expectation based solely on the dispersive nature of nonlinearly interacting kinetic Alfvén waves.
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Affiliation(s)
- Trevor A Bowen
- Space Sciences Laboratory, University of California, Berkeley, California 94720-7450, USA
| | - Alfred Mallet
- Space Sciences Laboratory, University of California, Berkeley, California 94720-7450, USA
| | - Stuart D Bale
- Space Sciences Laboratory, University of California, Berkeley, California 94720-7450, USA
- Physics Department, University of California, Berkeley, California 94720-7300, USA
- The Blackett Laboratory, Imperial College London, London SW7 2AZ, United Kingdom
- School of Physics and Astronomy, Queen Mary University of London, London E1 4NS, United Kingdom
| | - J W Bonnell
- Space Sciences Laboratory, University of California, Berkeley, California 94720-7450, USA
| | - Anthony W Case
- Smithsonian Astrophysical Observatory, Cambridge, Massachusetts 02138, USA
| | - Benjamin D G Chandran
- Department of Physics and Astronomy, University of New Hampshire, Durham, New Hampshire 03824, USA
- Space Science Center, University of New Hampshire, Durham, New Hampshire 03824, USA
| | - Alexandros Chasapis
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, Colorado 80303, USA
| | - Christopher H K Chen
- School of Physics and Astronomy, Queen Mary University of London, London E1 4NS, United Kingdom
| | - Die Duan
- Space Sciences Laboratory, University of California, Berkeley, California 94720-7450, USA
- School of Earth and Space Sciences, Peking University, Beijing 100871, China
| | - Thierry Dudok de Wit
- LPC2E, CNRS and University of Orléans, 3 Avenue de la Recherche Scientifique, 45071 Orléans, France
| | - Keith Goetz
- School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA
| | - Jasper S Halekas
- Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa 52242, USA
| | - Peter R Harvey
- Space Sciences Laboratory, University of California, Berkeley, California 94720-7450, USA
| | - J C Kasper
- Smithsonian Astrophysical Observatory, Cambridge, Massachusetts 02138, USA
- Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan 48109, USA
| | - Kelly E Korreck
- Smithsonian Astrophysical Observatory, Cambridge, Massachusetts 02138, USA
| | - Davin Larson
- Space Sciences Laboratory, University of California, Berkeley, California 94720-7450, USA
| | - Roberto Livi
- Space Sciences Laboratory, University of California, Berkeley, California 94720-7450, USA
| | - Robert J MacDowall
- Solar System Exploration Division, NASA/Goddard Space Flight Center, Greenbelt, Maryland 20771, USA
| | - David M Malaspina
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, Colorado 80303, USA
- Astrophysical and Planetary Sciences Department, University of Colorado, Boulder, Colorado, USA
| | - Michael D McManus
- Space Sciences Laboratory, University of California, Berkeley, California 94720-7450, USA
- Physics Department, University of California, Berkeley, California 94720-7300, USA
| | - Marc Pulupa
- Space Sciences Laboratory, University of California, Berkeley, California 94720-7450, USA
| | - Michael Stevens
- Smithsonian Astrophysical Observatory, Cambridge, Massachusetts 02138, USA
| | - Phyllis Whittlesey
- Space Sciences Laboratory, University of California, Berkeley, California 94720-7450, USA
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2
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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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3
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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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4
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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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5
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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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6
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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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8
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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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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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