Probing the Energetic Particle Environment near the Sun
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 accelerat...
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| Published in | Nature (London) Vol. 576; no. 7786; pp. 223 - 227 |
|---|---|
| Main Authors | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
| Format | Journal Article |
| Language | English |
| Published |
Goddard Space Flight Center
Nature Research
12.12.2019
Nature Publishing Group UK Nature Publishing Group |
| Subjects | |
| Online Access | Get full text |
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| 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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| AbstractList | NASA's Parker Solar Probe mission
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 ions
, and 'gradual' events
, 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 processes
. 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 spacecraft
. 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. 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. NASA's Parker Solar Probe mission.sup.1 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 ions.sup.2, and 'gradual' events.sup.3,4, 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 processes.sup.5. 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 spacecraft.sup.6. 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. NASA’s Parker Solar Probe mission 1 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 ions 2 , and ‘gradual’ events 3 , 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 processes 5 . 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 spacecraft 6 . 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. The Parker Solar Probe mission has reached the inner heliosphere of the Sun and made measurements of energetic particle events in the near-Sun radiation environment. 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 nearrelativistic 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. NASA's Parker Solar Probe mission.sup.1 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 ions.sup.2, and 'gradual' events.sup.3,4, 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 processes.sup.5. 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 spacecraft.sup.6. 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. The Parker Solar Probe mission has reached the inner heliosphere of the Sun and made measurements of energetic particle events in the near-Sun radiation environment. |
| Audience | PUBLIC Academic |
| Author | Rankin, J S Macdowall, R J Cummings, A C Bale, S D Korreck, K E Labrador, A W Case, A W Giacalone, J Schwadron, N A Roelof, E C Joyce, C J Rouillard, A P R L McNutt, Jr Mewaldt, R A Mccomas, D J Davis, A J Mitchell, D G Kasper, J C Krimigis, S M Szalay, J R Matthaeus, W H Cohen, C M S Desai, M I Posner, Arik Malandraki, O Leske, R A Pulupa, M Christian, E R Wiedenbeck, M E Stevens, M L Stone, E C Hill, M E |
| AuthorAffiliation | 1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 2 Goddard Space Flight Center, Greenbelt, MD 20771, USA 11 University of New Hampshire, Durham, NH 03824, USA 3 California Institute of Technology, Pasadena, CA 91125, USA 15 University of Michigan, Ann Arbor, MI 48109, USA 6 University of Arizona, Tucson, AZ 85721, USA 13 University of California at Berkeley, Berkeley, CA 94720, USA 14 The Blackett Laboratory Imperial College London, London, SW7 2AZ, UK 16 Smithsonian Astrophysical Observatory, Cambridge, MA 02138, USA 9 University of Delaware, Newark, DE 19716, USA 10 NASA HQ, Washington DC 20024, USA 12 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA 4 Southwest Research Institute, San Antonio, TX 78228, USA 7 Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA 8 National Observatory of Athens, IAASARS, Athens 15236 Greece 5 University of Texas at San Antonio, San Antonio, TX 78249, USA 17 CNRS, Toulou |
| AuthorAffiliation_xml | – name: 14 The Blackett Laboratory Imperial College London, London, SW7 2AZ, UK – name: 6 University of Arizona, Tucson, AZ 85721, USA – name: 10 NASA HQ, Washington DC 20024, USA – name: 5 University of Texas at San Antonio, San Antonio, TX 78249, USA – name: 1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA – name: 12 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA – name: 8 National Observatory of Athens, IAASARS, Athens 15236 Greece – name: 11 University of New Hampshire, Durham, NH 03824, USA – name: 16 Smithsonian Astrophysical Observatory, Cambridge, MA 02138, USA – name: 9 University of Delaware, Newark, DE 19716, USA – name: 2 Goddard Space Flight Center, Greenbelt, MD 20771, USA – name: 3 California Institute of Technology, Pasadena, CA 91125, USA – name: 13 University of California at Berkeley, Berkeley, CA 94720, USA – name: 15 University of Michigan, Ann Arbor, MI 48109, USA – name: 4 Southwest Research Institute, San Antonio, TX 78228, USA – name: 17 CNRS, Toulouse Cedex 4, France – name: 7 Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA |
| Author_xml | – sequence: 1 givenname: D J surname: Mccomas fullname: Mccomas, D J organization: Princeton University – sequence: 2 givenname: E R surname: Christian fullname: Christian, E R organization: Goddard Space Flight Center – sequence: 3 givenname: C M S surname: Cohen fullname: Cohen, C M S organization: Jet Propulsion Lab – sequence: 4 givenname: A C surname: Cummings fullname: Cummings, A C organization: Jet Propulsion Lab – sequence: 5 givenname: A J surname: Davis fullname: Davis, A J organization: Jet Propulsion Lab – sequence: 6 givenname: M I orcidid: 0000-0002-7318-6008 surname: Desai fullname: Desai, M I organization: Southwest Research Institute – sequence: 7 givenname: J surname: Giacalone fullname: Giacalone, J organization: University of Arizona – sequence: 8 givenname: M E surname: Hill fullname: Hill, M E organization: Johns Hopkins University Applied Physics Laboratory – sequence: 9 givenname: C J surname: Joyce fullname: Joyce, C J organization: Princeton University – sequence: 10 givenname: S M surname: Krimigis fullname: Krimigis, S M organization: Johns Hopkins University Applied Physics Laboratory – sequence: 11 givenname: A W surname: Labrador fullname: Labrador, A W organization: Jet Propulsion Lab – sequence: 12 givenname: R A surname: Leske fullname: Leske, R A organization: Jet Propulsion Lab – sequence: 13 givenname: O surname: Malandraki fullname: Malandraki, O organization: National Observatory of Athens – sequence: 14 givenname: W H surname: Matthaeus fullname: Matthaeus, W H organization: University of Delaware – sequence: 15 givenname: Jr surname: R L McNutt fullname: R L McNutt, Jr organization: Johns Hopkins University Applied Physics Laboratory – sequence: 16 givenname: R A surname: Mewaldt fullname: Mewaldt, R A organization: Jet Propulsion Lab – sequence: 17 givenname: D G surname: Mitchell fullname: Mitchell, D G organization: Johns Hopkins University Applied Physics Laboratory – sequence: 18 givenname: Arik surname: Posner fullname: Posner, Arik organization: National Aeronautics and Space Administration – sequence: 19 givenname: J S surname: Rankin fullname: Rankin, J S organization: Princeton University – sequence: 20 givenname: E C surname: Roelof fullname: Roelof, E C organization: Johns Hopkins University Applied Physics Laboratory – sequence: 21 givenname: N A surname: Schwadron fullname: Schwadron, N A organization: Princeton University – sequence: 22 givenname: E C surname: Stone fullname: Stone, E C organization: Jet Propulsion Lab – sequence: 23 givenname: J R orcidid: 0000-0003-2685-9801 surname: Szalay fullname: Szalay, J R organization: Princeton University – sequence: 24 givenname: M E surname: Wiedenbeck fullname: Wiedenbeck, M E organization: Jet Propulsion Lab – sequence: 25 givenname: S D surname: Bale fullname: Bale, S D organization: University of California, Berkeley – sequence: 26 givenname: J C surname: Kasper fullname: Kasper, J C organization: University of Michigan–Ann Arbor – sequence: 27 givenname: A W surname: Case fullname: Case, A W organization: Smithsonian Astrophysical Observatory – sequence: 28 givenname: K E surname: Korreck fullname: Korreck, K E organization: Smithsonian Astrophysical Observatory – sequence: 29 givenname: R J surname: Macdowall fullname: Macdowall, R J organization: Goddard Space Flight Center – sequence: 30 givenname: M surname: Pulupa fullname: Pulupa, M organization: University of California, Berkeley – sequence: 31 givenname: M L surname: Stevens fullname: Stevens, M L organization: Smithsonian Astrophysical Observatory – sequence: 32 givenname: A P surname: Rouillard fullname: Rouillard, A P organization: French National Centre for Scientific Research |
| BackLink | https://www.ncbi.nlm.nih.gov/pubmed/31802005$$D View this record in MEDLINE/PubMed |
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| ContentType | Journal Article |
| Copyright | Copyright Determination: GOV_PERMITTED The Author(s), under exclusive licence to Springer Nature Limited 2019 COPYRIGHT 2019 Nature Publishing Group Copyright Nature Publishing Group Dec 12, 2019 |
| Copyright_xml | – notice: Copyright Determination: GOV_PERMITTED – notice: The Author(s), under exclusive licence to Springer Nature Limited 2019 – notice: COPYRIGHT 2019 Nature Publishing Group – notice: Copyright Nature Publishing Group Dec 12, 2019 |
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| DOI | 10.1038/s41586-019-1811-1 |
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| Notes | GSFC GSFC-E-DAA-TN77243 Goddard Space Flight Center ObjectType-Article-1 SourceType-Scholarly Journals-1 ObjectType-Feature-2 content type line 23 Author Contributions D.J.M. is ISʘIS PI and led the data analysis and writing of study. E.R.C is ISʘIS Deputy PI, helped develop EPI-Hi, and participated in the data analysis. C.M.S.C helped develop EPI-Hi and participated in the data analysis. A.C.C. helped develop EPI-Hi and participated in the data analysis. A.J.D. helped develop EPI-Hi and participated in the data analysis. M.I.D. participated in the data analysis. J.G. participated in the data analysis. M.E.H helped develop EPI-Lo and participated in the data analysis. C.J.J. produced Figures 3 and 4 and participated in the data analysis. S.M.K. participated in the data analysis. A.W.L. helped develop EPI-Hi and participated in the data analysis. R.A.L. helped develop EPI-Hi and participated in the data analysis. O.M. participated in the data analysis. W.H.M participated in the data analysis. R.L.M. led the development of EPI-Lo and participated in the data analysis. R.A.M helped develop EPI-Hi and participated in the data analysis. D.G.M. helped develop EPI-Lo and participated in the data analysis. A.P. participated in the data analysis. J.S.R. helped develop EPI-Hi and participated in the data analysis. E.C.R. participated in the data analysis. N.A.S. led the development of the ISʘIS SOC and participated in the data analysis. E.C.S. helped develop EPI-Hi and participated in the data analysis. J.R.S. led the development of the analysis tool, produced Figures 1 and 2, and participated in the data analysis. M.E.W. led the development of EPI-Hi and participated in the data analysis. S.D.B. is FIELDS PI and participated in the data analysis. J.C.K. is SWEAP PI and participated in the data analysis. A.W.C. helped develop SWEAP and participated in the data analysis. K.E.K. helped develop SWEAP and participated in the data analysis. R.J.M. helped develop FIELDS and participated in the data analysis. M.P. helped develop FIELDS and participated in the data analysis. M.L.S. helped develop SWEAP and participated in the data analysis. A.P.R. led the CME simulation work and participated in the data analysis. |
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| References | Cane, Richardson, von Rosenvinge (CR5) 2010; 115 McComas (CR7) 2016; 204 Richardson, von Rosenvinge, Cane (CR21) 2015; 290 Fox (CR1) 2016; 204 Rouillard (CR28) 2010; 114 CR14 CR13 Bučik (CR24) 2014; 786 Bale (CR9) 2016; 204 Wood, Howard (CR29) 2009; 702 Vourlidas (CR10) 2016; 204 Chotoo (CR16) 2000; 105 Bučik (CR23) 2018; 869 Mason (CR2) 2007; 130 Wiedenbeck (CR22) 2013; 762 Isavnin (CR30) 2016; 833 CR4 Zwickl, Roelof, Gold, Krimigis, Armstrong (CR18) 1978; 225 Gosling (CR12) 1996; 34 Reinhard, Wibberenz (CR19) 1974; 36 Wibberenz, Cane (CR6) 2006; 650 Thernisien, Vourlidas, Howard (CR27) 2009; 256 Giacalone, Jokipii, Kota (CR17) 2002; 573 Desai, Giacalone (CR3) 2016; 13 Kasper (CR8) 2016; 204 Kouloumvakos (CR15) 2019; 876 Pizzo (CR11) 1978; 83 Kallenrode (CR20) 1993; 98 Howard (CR26) 2002; 29 Nitta, Mason, Wang, Cohen, Wiedenbeck (CR25) 2015; 806 31802020 - Nature. 2019 Dec;576(7785):15-16 31822830 - Nature. 2019 Dec;576(7786):219-220 R Bučik (1811_CR24) 2014; 786 A Vourlidas (1811_CR10) 2016; 204 RA Howard (1811_CR26) 2002; 29 JC Kasper (1811_CR8) 2016; 204 DJ McComas (1811_CR7) 2016; 204 V Pizzo (1811_CR11) 1978; 83 SD Bale (1811_CR9) 2016; 204 R Bučik (1811_CR23) 2018; 869 G Wibberenz (1811_CR6) 2006; 650 J Gosling (1811_CR12) 1996; 34 IG Richardson (1811_CR21) 2015; 290 NJ Fox (1811_CR1) 2016; 204 1811_CR4 HV Cane (1811_CR5) 2010; 115 RD Zwickl (1811_CR18) 1978; 225 R Reinhard (1811_CR19) 1974; 36 A Isavnin (1811_CR30) 2016; 833 NV Nitta (1811_CR25) 2015; 806 K Chotoo (1811_CR16) 2000; 105 1811_CR13 GM Mason (1811_CR2) 2007; 130 1811_CR14 A Kouloumvakos (1811_CR15) 2019; 876 ME Wiedenbeck (1811_CR22) 2013; 762 MI Desai (1811_CR3) 2016; 13 MB Kallenrode (1811_CR20) 1993; 98 B Wood (1811_CR29) 2009; 702 J Giacalone (1811_CR17) 2002; 573 A Thernisien (1811_CR27) 2009; 256 AP Rouillard (1811_CR28) 2010; 114 |
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| Snippet | 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.... NASA’s Parker Solar Probe mission 1 recently plunged through the inner heliosphere of the Sun to its perihelia, about 24 million kilometres from the Sun.... NASA's Parker Solar Probe mission recently plunged through the inner heliosphere of the Sun to its perihelia, about 24 million kilometres from the Sun.... NASA's Parker Solar Probe mission.sup.1 recently plunged through the inner heliosphere of the Sun to its perihelia, about 24 million kilometres from the Sun.... 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.... |
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| SubjectTerms | 639/766/34/866 639/766/525/870 Celestial bodies Corona Coronal mass ejection Corotating Interaction Regions (CIR) Energetic particles Energetics Energy Heliosphere Helium Humanities and Social Sciences Magnetic fields Magnetic reconnection Measurement multidisciplinary Observations Orbits Particle acceleration Protons Radiation Science Science (multidisciplinary) Solar energetic particles Solar flares Solar Physics Solar probes Solar wind Space probes Sun Transport |
| Title | Probing the Energetic Particle Environment near the Sun |
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