Pluto's Interaction With Energetic Heliospheric Ions
Pluto energies of a few kiloelectron volts and suprathermal ions with tens of kiloelectron volts and above. We measure this population using the Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) instrument on board the New Horizons spacecraft that flew by Pluto in 2015. Even thoug...
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Veröffentlicht in: | Journal of geophysical research. Space physics 2019-09, Vol.124 (9), p.7413-7424 |
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creator | Kollmann, P. Hill, M. E. Allen, R. C. McNutt, R. L. Brown, L. E. Barnes, N. P. Delamere, P. Clark, G. Andrews, G. B. Salazar, N. Westlake, J. Romeo, G. Vandegriff, J. Kusterer, M. Smith, D. Nelson, K. Jaskulek, S. Decker, R. B. Cheng, A. F. Krimigis, S. M. Lisse, C. M. Mitchell, D. G. Weaver, H. A. Elliott, H. A. Fattig, E. Gladstone, G. R. Valek, P. W. Weidner, S. Kammer, J. Bagenal, F. Horanyi, M. Kaufmann, D. Harch, A. Olkin, C. B. Piquette, M. R. Spencer, J. R. Young, L. A. Ennico, K. Summers, M. E. Stern, S. A. |
description | Pluto energies of a few kiloelectron volts and suprathermal ions with tens of kiloelectron volts and above. We measure this population using the Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) instrument on board the New Horizons spacecraft that flew by Pluto in 2015. Even though the measured ions have gyroradii larger than the size of Pluto and the cross section of its magnetosphere, we find that the boundary of the magnetosphere is depleting the energetic ion intensities by about an order of magnitude close to Pluto. The intensity is increasing exponentially with distance to Pluto and reaches nominal levels of the interplanetary medium at about 190RP distance. Inside the wake of Pluto, we observe oscillations of the ion intensities with a periodicity of about 0.2 hr. We show that these can be quantitatively explained by the electric field of an ultralow‐frequency wave and discuss possible physical drivers for such a field. We find no evidence for the presence of plutogenic ions in the considered energy range.
Plain Language Summary
Space around Pluto is not entirely empty but filled with solar wind plasma and ions that originate from interstellar space and are pushed outward by the solar wind. All planetary bodies interact with their surrounding medium. In the case of a magnetized body like Earth, this interaction is strong and creates a magnetosphere. Unmagnetized bodies like that of the dwarf planet Pluto have a much weaker interaction. What makes Pluto special is that it is far outside in our solar system and therefore embedded in relatively high intensities of interstellar ions. When New Horizons passed Pluto and measured the distribution of these ions, we found that Pluto is forming a wake in the interstellar ion flow. It is more difficult to deflect the motion of the relatively fast‐moving interstellar ions than it is to deflect the lower‐energy solar wind. Therefore, it was not obvious that we would observe this. Even Pluto's wake is not entirely empty because some interstellar ions do manage to enter. Another finding was that a wave is propagating within the tenuous medium of the wake. This wave modulates the ion intensities resembling a sound wave propagating through air and modulating the gas density.
Key Points
Pluto forms a wake for energetic heliospheric ions
Waves cause ion intensity oscillations in the wake |
doi_str_mv | 10.1029/2019JA026830 |
format | Article |
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Plain Language Summary
Space around Pluto is not entirely empty but filled with solar wind plasma and ions that originate from interstellar space and are pushed outward by the solar wind. All planetary bodies interact with their surrounding medium. In the case of a magnetized body like Earth, this interaction is strong and creates a magnetosphere. Unmagnetized bodies like that of the dwarf planet Pluto have a much weaker interaction. What makes Pluto special is that it is far outside in our solar system and therefore embedded in relatively high intensities of interstellar ions. When New Horizons passed Pluto and measured the distribution of these ions, we found that Pluto is forming a wake in the interstellar ion flow. It is more difficult to deflect the motion of the relatively fast‐moving interstellar ions than it is to deflect the lower‐energy solar wind. Therefore, it was not obvious that we would observe this. Even Pluto's wake is not entirely empty because some interstellar ions do manage to enter. Another finding was that a wave is propagating within the tenuous medium of the wake. This wave modulates the ion intensities resembling a sound wave propagating through air and modulating the gas density.
Key Points
Pluto forms a wake for energetic heliospheric ions
Waves cause ion intensity oscillations in the wake</description><identifier>ISSN: 2169-9380</identifier><identifier>EISSN: 2169-9402</identifier><identifier>DOI: 10.1029/2019JA026830</identifier><identifier>PMID: 35860291</identifier><language>eng</language><publisher>Washington: Blackwell Publishing Ltd</publisher><subject>Dwarf planets ; Earth magnetosphere ; Electric fields ; Embedded systems ; Energetic Particles ; Gas density ; Interplanetary medium ; Interplanetary Physics ; Interstellar space ; Ionosphere ; Ions ; Magnetospheres ; Magnetospheric Physics ; New Horizons ; New Horizons mission ; Periodic variations ; Pickup Ions ; Planetary Magnetospheres ; Planetary Sciences: Comets and Small Bodies ; Plasma Waves and Instabilities ; Pluto ; Pluto (dwarf planet) ; Solar energy ; Solar Physics, Astrophysics, and Astronomy ; Solar system ; Solar wind ; Solar Wind Interactions with Unmagnetized Bodies ; Sound propagation ; Sound waves ; Spacecraft ; wave ; Wave propagation</subject><ispartof>Journal of geophysical research. Space physics, 2019-09, Vol.124 (9), p.7413-7424</ispartof><rights>2019. The Authors.</rights><rights>2019. American Geophysical Union. All Rights Reserved.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c4338-bc46836ff3c4bc56ae773911558bfdd7d23706e61ca3666d098bd6d1720e653e3</citedby><cites>FETCH-LOGICAL-c4338-bc46836ff3c4bc56ae773911558bfdd7d23706e61ca3666d098bd6d1720e653e3</cites><orcidid>0000-0003-0472-8640 ; 0000-0002-9608-8646 ; 0000-0002-9171-0862 ; 0000-0003-2079-5683 ; 0000-0002-3441-3757 ; 0000-0002-5264-7194 ; 0000-0002-2318-8750 ; 0000-0002-0655-9863 ; 0000-0002-4722-9166 ; 0000-0002-8847-8492 ; 0000-0002-9548-1526 ; 0000-0002-5505-0510 ; 0000-0002-7547-3967 ; 0000-0003-4452-8109 ; 0000-0001-5375-4250 ; 0000-0003-0060-072X ; 0000-0002-3963-1614 ; 0000-0002-5846-716X ; 0000-0003-1098-9759 ; 0000-0003-1960-2119 ; 0000-0002-4274-9760 ; 0000-0003-0951-7762 ; 0000-0003-2297-3922 ; 0000-0001-5986-8902 ; 0000-0001-5018-7537 ; 0000-0002-5674-4936 ; 0000-0002-0781-1565 ; 0000-0002-0190-3194</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://onlinelibrary.wiley.com/doi/pdf/10.1029%2F2019JA026830$$EPDF$$P50$$Gwiley$$Hfree_for_read</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1029%2F2019JA026830$$EHTML$$P50$$Gwiley$$Hfree_for_read</linktohtml><link.rule.ids>230,314,776,780,881,1411,1427,27901,27902,45550,45551,46384,46808</link.rule.ids></links><search><creatorcontrib>Kollmann, P.</creatorcontrib><creatorcontrib>Hill, M. E.</creatorcontrib><creatorcontrib>Allen, R. C.</creatorcontrib><creatorcontrib>McNutt, R. L.</creatorcontrib><creatorcontrib>Brown, L. E.</creatorcontrib><creatorcontrib>Barnes, N. P.</creatorcontrib><creatorcontrib>Delamere, P.</creatorcontrib><creatorcontrib>Clark, G.</creatorcontrib><creatorcontrib>Andrews, G. B.</creatorcontrib><creatorcontrib>Salazar, N.</creatorcontrib><creatorcontrib>Westlake, J.</creatorcontrib><creatorcontrib>Romeo, G.</creatorcontrib><creatorcontrib>Vandegriff, J.</creatorcontrib><creatorcontrib>Kusterer, M.</creatorcontrib><creatorcontrib>Smith, D.</creatorcontrib><creatorcontrib>Nelson, K.</creatorcontrib><creatorcontrib>Jaskulek, S.</creatorcontrib><creatorcontrib>Decker, R. B.</creatorcontrib><creatorcontrib>Cheng, A. F.</creatorcontrib><creatorcontrib>Krimigis, S. M.</creatorcontrib><creatorcontrib>Lisse, C. M.</creatorcontrib><creatorcontrib>Mitchell, D. G.</creatorcontrib><creatorcontrib>Weaver, H. A.</creatorcontrib><creatorcontrib>Elliott, H. A.</creatorcontrib><creatorcontrib>Fattig, E.</creatorcontrib><creatorcontrib>Gladstone, G. R.</creatorcontrib><creatorcontrib>Valek, P. W.</creatorcontrib><creatorcontrib>Weidner, S.</creatorcontrib><creatorcontrib>Kammer, J.</creatorcontrib><creatorcontrib>Bagenal, F.</creatorcontrib><creatorcontrib>Horanyi, M.</creatorcontrib><creatorcontrib>Kaufmann, D.</creatorcontrib><creatorcontrib>Harch, A.</creatorcontrib><creatorcontrib>Olkin, C. B.</creatorcontrib><creatorcontrib>Piquette, M. R.</creatorcontrib><creatorcontrib>Spencer, J. R.</creatorcontrib><creatorcontrib>Young, L. A.</creatorcontrib><creatorcontrib>Ennico, K.</creatorcontrib><creatorcontrib>Summers, M. E.</creatorcontrib><creatorcontrib>Stern, S. A.</creatorcontrib><title>Pluto's Interaction With Energetic Heliospheric Ions</title><title>Journal of geophysical research. Space physics</title><description>Pluto energies of a few kiloelectron volts and suprathermal ions with tens of kiloelectron volts and above. We measure this population using the Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) instrument on board the New Horizons spacecraft that flew by Pluto in 2015. Even though the measured ions have gyroradii larger than the size of Pluto and the cross section of its magnetosphere, we find that the boundary of the magnetosphere is depleting the energetic ion intensities by about an order of magnitude close to Pluto. The intensity is increasing exponentially with distance to Pluto and reaches nominal levels of the interplanetary medium at about 190RP distance. Inside the wake of Pluto, we observe oscillations of the ion intensities with a periodicity of about 0.2 hr. We show that these can be quantitatively explained by the electric field of an ultralow‐frequency wave and discuss possible physical drivers for such a field. We find no evidence for the presence of plutogenic ions in the considered energy range.
Plain Language Summary
Space around Pluto is not entirely empty but filled with solar wind plasma and ions that originate from interstellar space and are pushed outward by the solar wind. All planetary bodies interact with their surrounding medium. In the case of a magnetized body like Earth, this interaction is strong and creates a magnetosphere. Unmagnetized bodies like that of the dwarf planet Pluto have a much weaker interaction. What makes Pluto special is that it is far outside in our solar system and therefore embedded in relatively high intensities of interstellar ions. When New Horizons passed Pluto and measured the distribution of these ions, we found that Pluto is forming a wake in the interstellar ion flow. It is more difficult to deflect the motion of the relatively fast‐moving interstellar ions than it is to deflect the lower‐energy solar wind. Therefore, it was not obvious that we would observe this. Even Pluto's wake is not entirely empty because some interstellar ions do manage to enter. Another finding was that a wave is propagating within the tenuous medium of the wake. This wave modulates the ion intensities resembling a sound wave propagating through air and modulating the gas density.
Key Points
Pluto forms a wake for energetic heliospheric ions
Waves cause ion intensity oscillations in the wake</description><subject>Dwarf planets</subject><subject>Earth magnetosphere</subject><subject>Electric fields</subject><subject>Embedded systems</subject><subject>Energetic Particles</subject><subject>Gas density</subject><subject>Interplanetary medium</subject><subject>Interplanetary Physics</subject><subject>Interstellar space</subject><subject>Ionosphere</subject><subject>Ions</subject><subject>Magnetospheres</subject><subject>Magnetospheric Physics</subject><subject>New Horizons</subject><subject>New Horizons mission</subject><subject>Periodic variations</subject><subject>Pickup Ions</subject><subject>Planetary Magnetospheres</subject><subject>Planetary Sciences: Comets and Small Bodies</subject><subject>Plasma Waves and Instabilities</subject><subject>Pluto</subject><subject>Pluto (dwarf planet)</subject><subject>Solar energy</subject><subject>Solar Physics, Astrophysics, and Astronomy</subject><subject>Solar system</subject><subject>Solar wind</subject><subject>Solar Wind Interactions with Unmagnetized Bodies</subject><subject>Sound propagation</subject><subject>Sound waves</subject><subject>Spacecraft</subject><subject>wave</subject><subject>Wave propagation</subject><issn>2169-9380</issn><issn>2169-9402</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><sourceid>24P</sourceid><recordid>eNp9kUtLAzEQx4MoVqo3P0DBgx6s5rF5XYRSqq0Iiigew252to1sNzXZVfz2plRFPTiXef3mzwyD0CHBZwRTfU4x0dcjTIVieAvtUSL0UGeYbn_FTOEeOojxGSdTqUT4LuoxrkQaJ3sou6u71h_HwaxpIeS2db4ZPLl2MZg0EObQOjuYQu18XC0gpGTmm7iPdqq8jnDw6fvo8XLyMJ4Ob26vZuPRzdBmjKlhYbO0l6gqZrPCcpGDlEwTwrkqqrKUJWUSCxDE5kwIUWKtilKURFIMgjNgfXSx0V11xRJKC00b8tqsglvm4d343JnfncYtzNy_Gk0VlzRLAiefAsG_dBBbs3TRQl3nDfguGio0lTzTVCf06A_67LvQpPMMZVjKTCmyFjzdUDb4GANU38sQbNYfMT8_knC2wd9cDe__sub66n7EOVGKfQAQHolj</recordid><startdate>201909</startdate><enddate>201909</enddate><creator>Kollmann, P.</creator><creator>Hill, M. 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E. ; Allen, R. C. ; McNutt, R. L. ; Brown, L. E. ; Barnes, N. P. ; Delamere, P. ; Clark, G. ; Andrews, G. B. ; Salazar, N. ; Westlake, J. ; Romeo, G. ; Vandegriff, J. ; Kusterer, M. ; Smith, D. ; Nelson, K. ; Jaskulek, S. ; Decker, R. B. ; Cheng, A. F. ; Krimigis, S. M. ; Lisse, C. M. ; Mitchell, D. G. ; Weaver, H. A. ; Elliott, H. A. ; Fattig, E. ; Gladstone, G. R. ; Valek, P. W. ; Weidner, S. ; Kammer, J. ; Bagenal, F. ; Horanyi, M. ; Kaufmann, D. ; Harch, A. ; Olkin, C. B. ; Piquette, M. R. ; Spencer, J. R. ; Young, L. A. ; Ennico, K. ; Summers, M. E. ; Stern, S. 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A.</creatorcontrib><collection>Wiley-Blackwell Open Access Collection</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>MEDLINE - Academic</collection><collection>PubMed Central (Full Participant titles)</collection><jtitle>Journal of geophysical research. Space physics</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Kollmann, P.</au><au>Hill, M. E.</au><au>Allen, R. C.</au><au>McNutt, R. L.</au><au>Brown, L. E.</au><au>Barnes, N. P.</au><au>Delamere, P.</au><au>Clark, G.</au><au>Andrews, G. B.</au><au>Salazar, N.</au><au>Westlake, J.</au><au>Romeo, G.</au><au>Vandegriff, J.</au><au>Kusterer, M.</au><au>Smith, D.</au><au>Nelson, K.</au><au>Jaskulek, S.</au><au>Decker, R. B.</au><au>Cheng, A. F.</au><au>Krimigis, S. M.</au><au>Lisse, C. M.</au><au>Mitchell, D. G.</au><au>Weaver, H. A.</au><au>Elliott, H. A.</au><au>Fattig, E.</au><au>Gladstone, G. R.</au><au>Valek, P. W.</au><au>Weidner, S.</au><au>Kammer, J.</au><au>Bagenal, F.</au><au>Horanyi, M.</au><au>Kaufmann, D.</au><au>Harch, A.</au><au>Olkin, C. B.</au><au>Piquette, M. R.</au><au>Spencer, J. R.</au><au>Young, L. A.</au><au>Ennico, K.</au><au>Summers, M. E.</au><au>Stern, S. A.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Pluto's Interaction With Energetic Heliospheric Ions</atitle><jtitle>Journal of geophysical research. Space physics</jtitle><date>2019-09</date><risdate>2019</risdate><volume>124</volume><issue>9</issue><spage>7413</spage><epage>7424</epage><pages>7413-7424</pages><issn>2169-9380</issn><eissn>2169-9402</eissn><abstract>Pluto energies of a few kiloelectron volts and suprathermal ions with tens of kiloelectron volts and above. We measure this population using the Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) instrument on board the New Horizons spacecraft that flew by Pluto in 2015. Even though the measured ions have gyroradii larger than the size of Pluto and the cross section of its magnetosphere, we find that the boundary of the magnetosphere is depleting the energetic ion intensities by about an order of magnitude close to Pluto. The intensity is increasing exponentially with distance to Pluto and reaches nominal levels of the interplanetary medium at about 190RP distance. Inside the wake of Pluto, we observe oscillations of the ion intensities with a periodicity of about 0.2 hr. We show that these can be quantitatively explained by the electric field of an ultralow‐frequency wave and discuss possible physical drivers for such a field. We find no evidence for the presence of plutogenic ions in the considered energy range.
Plain Language Summary
Space around Pluto is not entirely empty but filled with solar wind plasma and ions that originate from interstellar space and are pushed outward by the solar wind. All planetary bodies interact with their surrounding medium. In the case of a magnetized body like Earth, this interaction is strong and creates a magnetosphere. Unmagnetized bodies like that of the dwarf planet Pluto have a much weaker interaction. What makes Pluto special is that it is far outside in our solar system and therefore embedded in relatively high intensities of interstellar ions. When New Horizons passed Pluto and measured the distribution of these ions, we found that Pluto is forming a wake in the interstellar ion flow. It is more difficult to deflect the motion of the relatively fast‐moving interstellar ions than it is to deflect the lower‐energy solar wind. Therefore, it was not obvious that we would observe this. Even Pluto's wake is not entirely empty because some interstellar ions do manage to enter. Another finding was that a wave is propagating within the tenuous medium of the wake. This wave modulates the ion intensities resembling a sound wave propagating through air and modulating the gas density.
Key Points
Pluto forms a wake for energetic heliospheric ions
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fulltext | fulltext |
identifier | ISSN: 2169-9380 |
ispartof | Journal of geophysical research. Space physics, 2019-09, Vol.124 (9), p.7413-7424 |
issn | 2169-9380 2169-9402 |
language | eng |
recordid | cdi_pubmedcentral_primary_oai_pubmedcentral_nih_gov_9285724 |
source | Wiley Online Library; Wiley Online Library Journals Frontfile Complete |
subjects | Dwarf planets Earth magnetosphere Electric fields Embedded systems Energetic Particles Gas density Interplanetary medium Interplanetary Physics Interstellar space Ionosphere Ions Magnetospheres Magnetospheric Physics New Horizons New Horizons mission Periodic variations Pickup Ions Planetary Magnetospheres Planetary Sciences: Comets and Small Bodies Plasma Waves and Instabilities Pluto Pluto (dwarf planet) Solar energy Solar Physics, Astrophysics, and Astronomy Solar system Solar wind Solar Wind Interactions with Unmagnetized Bodies Sound propagation Sound waves Spacecraft wave Wave propagation |
title | Pluto's Interaction With Energetic Heliospheric Ions |
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