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Jupiter's Whistler‐Mode Belts and Electron Slot Region
The spatial distribution of whistler‐mode wave emissions in the Jovian magnetosphere measured during the first 45 perijove orbits of Juno is investigated. A double‐belt structure in whistler‐mode wave intensity is revealed. Between the two whistler‐mode belts, there exists a region devoid of 100 s k...
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| Published in: | Journal of geophysical research. Space physics 2024-12, Vol.129 (12), p.n/a |
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| container_title | Journal of geophysical research. Space physics |
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| creator | Hao, Y.‐X. Shprits, Y. Y. Menietti, J. D. Liu, Z. Y. Averkamp, T. Wang, D. D. Kollmann, P. Hospodarsky, G. B. Drozdov, A. Roussos, E. Krupp, N. Horne, R. B. Woodfield, E. E. Bolton, S. J. |
| description | The spatial distribution of whistler‐mode wave emissions in the Jovian magnetosphere measured during the first 45 perijove orbits of Juno is investigated. A double‐belt structure in whistler‐mode wave intensity is revealed. Between the two whistler‐mode belts, there exists a region devoid of 100 s keV electrons near the magnetic equator at 9 |
| doi_str_mv | 10.1029/2024JA032850 |
| format | article |
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Plain Language Summary
Whistler‐mode waves act as a potential driver of energetic electron dynamics in the Jovian magnetosphere. By resonating with the gyro‐bounce motion of electrons along the field line, whistler‐mode waves lead to either the acceleration of electrons or their precipitation to the atmosphere. Quantifying the net effect of such waves toward the radiation belt of Jupiter requires a comprehensive knowledge of how wavers are distributed in the Jovian magnetosphere. With NASA's Juno mission, we reveal a novel double‐belt distribution of the whistler‐mode waves. Between the inner and outer whistler‐mode belts there is a region lacking near‐equatorial energetic (100 s keV) electrons. The outer whistler‐mode belt seems to be a mixture of chorus waves generated near the equator and auroral hiss waves propagating from the polar region. Either more abundant source electrons at the duskside magnetic equator for chorus emission or stronger auroral hiss from the duskside polar region can explain the dawn‐dusk asymmetry of the outer whistler‐mode belt.
Key Points
A double‐belt structure in Jovian whistler‐mode wave (>0.1 fceq) intensity is revealed
Near‐equatorial energetic electron distributions measured by JEDI show similar radial and azimuthal profile as whistler‐mode waves
The dawn‐dusk asymmetry in the outer whistler‐mode belt intensity corresponds to either the abundance of source electrons or auroral hiss</description><identifier>ISSN: 2169-9380</identifier><identifier>EISSN: 2169-9402</identifier><identifier>DOI: 10.1029/2024JA032850</identifier><language>eng</language><publisher>Washington: Blackwell Publishing Ltd</publisher><subject>Auroral hiss ; Chorus waves ; Electron distribution ; Electrons ; Emission ; Emission measurements ; Equatorial regions ; galileon moons ; Hiss ; Jupiter ; Jupiter atmosphere ; Jupiter probes ; Magnetic equator ; Orbits ; Planetary magnetospheres ; Polar environments ; Polar regions ; Propagation modes ; radiation belt ; Radiation belts ; Solar cycle ; Space missions ; Spatial distribution ; Wave propagation ; wave‐particle interaction ; Whistlers ; whistler‐mode waves</subject><ispartof>Journal of geophysical research. Space physics, 2024-12, Vol.129 (12), p.n/a</ispartof><rights>2024. The Author(s).</rights><rights>2024. This article is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c2328-a481b8e10874bf476af120cf6381ce141876f3dc3b4fa61a2aee1c8a9e57703</cites><orcidid>0000-0003-4683-9533 ; 0000-0002-9625-0834 ; 0000-0002-9115-0789 ; 0000-0002-0412-6407 ; 0000-0002-5699-0678 ; 0000-0001-9200-9878 ; 0000-0001-6977-3472 ; 0000-0002-5334-2026 ; 0000-0002-0531-8814 ; 0000-0003-0425-3358 ; 0000-0001-6737-251X ; 0000-0002-4213-4037 ; 0000-0002-4274-9760</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,777,781,27905,27906</link.rule.ids></links><search><creatorcontrib>Hao, Y.‐X.</creatorcontrib><creatorcontrib>Shprits, Y. Y.</creatorcontrib><creatorcontrib>Menietti, J. D.</creatorcontrib><creatorcontrib>Liu, Z. Y.</creatorcontrib><creatorcontrib>Averkamp, T.</creatorcontrib><creatorcontrib>Wang, D. D.</creatorcontrib><creatorcontrib>Kollmann, P.</creatorcontrib><creatorcontrib>Hospodarsky, G. B.</creatorcontrib><creatorcontrib>Drozdov, A.</creatorcontrib><creatorcontrib>Roussos, E.</creatorcontrib><creatorcontrib>Krupp, N.</creatorcontrib><creatorcontrib>Horne, R. B.</creatorcontrib><creatorcontrib>Woodfield, E. E.</creatorcontrib><creatorcontrib>Bolton, S. J.</creatorcontrib><title>Jupiter's Whistler‐Mode Belts and Electron Slot Region</title><title>Journal of geophysical research. Space physics</title><description>The spatial distribution of whistler‐mode wave emissions in the Jovian magnetosphere measured during the first 45 perijove orbits of Juno is investigated. A double‐belt structure in whistler‐mode wave intensity is revealed. Between the two whistler‐mode belts, there exists a region devoid of 100 s keV electrons near the magnetic equator at 9<M<16 $9< M< 16$. Insufficient source electron population in such an electron “slot” region is a possible explanation for the relatively lower wave activity compared to the whistler‐mode belts. The wave intensity of the outer whistler‐mode belt measured in the dusk‐premidnight sector is significantly stronger than in the postmidnight‐dawn sector. We suggest that the inherent dawn‐dusk asymmetries in source electron distribution and/or auroral hiss emission rather than the modulation of solar cycle are more likely to result in the azimuthal variation of outer whistler‐mode belt intensity during the first 45 Juno perijove orbits.
Plain Language Summary
Whistler‐mode waves act as a potential driver of energetic electron dynamics in the Jovian magnetosphere. By resonating with the gyro‐bounce motion of electrons along the field line, whistler‐mode waves lead to either the acceleration of electrons or their precipitation to the atmosphere. Quantifying the net effect of such waves toward the radiation belt of Jupiter requires a comprehensive knowledge of how wavers are distributed in the Jovian magnetosphere. With NASA's Juno mission, we reveal a novel double‐belt distribution of the whistler‐mode waves. Between the inner and outer whistler‐mode belts there is a region lacking near‐equatorial energetic (100 s keV) electrons. The outer whistler‐mode belt seems to be a mixture of chorus waves generated near the equator and auroral hiss waves propagating from the polar region. Either more abundant source electrons at the duskside magnetic equator for chorus emission or stronger auroral hiss from the duskside polar region can explain the dawn‐dusk asymmetry of the outer whistler‐mode belt.
Key Points
A double‐belt structure in Jovian whistler‐mode wave (>0.1 fceq) intensity is revealed
Near‐equatorial energetic electron distributions measured by JEDI show similar radial and azimuthal profile as whistler‐mode waves
The dawn‐dusk asymmetry in the outer whistler‐mode belt intensity corresponds to either the abundance of source electrons or auroral hiss</description><subject>Auroral hiss</subject><subject>Chorus waves</subject><subject>Electron distribution</subject><subject>Electrons</subject><subject>Emission</subject><subject>Emission measurements</subject><subject>Equatorial regions</subject><subject>galileon moons</subject><subject>Hiss</subject><subject>Jupiter</subject><subject>Jupiter atmosphere</subject><subject>Jupiter probes</subject><subject>Magnetic equator</subject><subject>Orbits</subject><subject>Planetary magnetospheres</subject><subject>Polar environments</subject><subject>Polar regions</subject><subject>Propagation modes</subject><subject>radiation belt</subject><subject>Radiation belts</subject><subject>Solar cycle</subject><subject>Space missions</subject><subject>Spatial distribution</subject><subject>Wave propagation</subject><subject>wave‐particle interaction</subject><subject>Whistlers</subject><subject>whistler‐mode waves</subject><issn>2169-9380</issn><issn>2169-9402</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>24P</sourceid><recordid>eNp9kMFKAzEQhoMoWLQ3H2DBgxdXM0l2d_ZYS62WitAKHkO6neiWdVOTLdKbj-Az-iRGquDJucwwfPzzz8_YCfAL4KK8FFyoyYBLgRnfYz0BeZmWiov931kiP2T9EFY8FsYVZD2Gk8267sifheTxuQ5dQ_7z_ePOLSm5oqYLiWmXyaihqvOuTeaN65IZPdWuPWYH1jSB-j_9iM2vRw_Dm3R6P74dDqZpJaKV1CiEBRJwLNTCqiI3FgSvbC4RKgIFWORWLiu5UNbkYIQhggpNSVlRcHnETneqa-9eNxQ6vXIb38aDWoJClcdny0id76jKuxA8Wb329YvxWw1cf4ej_4YTcbnD3-qGtv-yejKeDTJEhfILy2FkPA</recordid><startdate>202412</startdate><enddate>202412</enddate><creator>Hao, Y.‐X.</creator><creator>Shprits, Y. Y.</creator><creator>Menietti, J. D.</creator><creator>Liu, Z. Y.</creator><creator>Averkamp, T.</creator><creator>Wang, D. D.</creator><creator>Kollmann, P.</creator><creator>Hospodarsky, G. B.</creator><creator>Drozdov, A.</creator><creator>Roussos, E.</creator><creator>Krupp, N.</creator><creator>Horne, R. B.</creator><creator>Woodfield, E. E.</creator><creator>Bolton, S. J.</creator><general>Blackwell Publishing Ltd</general><scope>24P</scope><scope>WIN</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0003-4683-9533</orcidid><orcidid>https://orcid.org/0000-0002-9625-0834</orcidid><orcidid>https://orcid.org/0000-0002-9115-0789</orcidid><orcidid>https://orcid.org/0000-0002-0412-6407</orcidid><orcidid>https://orcid.org/0000-0002-5699-0678</orcidid><orcidid>https://orcid.org/0000-0001-9200-9878</orcidid><orcidid>https://orcid.org/0000-0001-6977-3472</orcidid><orcidid>https://orcid.org/0000-0002-5334-2026</orcidid><orcidid>https://orcid.org/0000-0002-0531-8814</orcidid><orcidid>https://orcid.org/0000-0003-0425-3358</orcidid><orcidid>https://orcid.org/0000-0001-6737-251X</orcidid><orcidid>https://orcid.org/0000-0002-4213-4037</orcidid><orcidid>https://orcid.org/0000-0002-4274-9760</orcidid></search><sort><creationdate>202412</creationdate><title>Jupiter's Whistler‐Mode Belts and Electron Slot Region</title><author>Hao, Y.‐X. ; Shprits, Y. Y. ; Menietti, J. D. ; Liu, Z. Y. ; Averkamp, T. ; Wang, D. D. ; Kollmann, P. ; Hospodarsky, G. B. ; Drozdov, A. ; Roussos, E. ; Krupp, N. ; Horne, R. B. ; Woodfield, E. E. ; Bolton, S. 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J.</creatorcontrib><collection>Wiley Online Library Open Access</collection><collection>Wiley Online Library Open Access</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><jtitle>Journal of geophysical research. Space physics</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Hao, Y.‐X.</au><au>Shprits, Y. Y.</au><au>Menietti, J. D.</au><au>Liu, Z. Y.</au><au>Averkamp, T.</au><au>Wang, D. D.</au><au>Kollmann, P.</au><au>Hospodarsky, G. B.</au><au>Drozdov, A.</au><au>Roussos, E.</au><au>Krupp, N.</au><au>Horne, R. B.</au><au>Woodfield, E. E.</au><au>Bolton, S. J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Jupiter's Whistler‐Mode Belts and Electron Slot Region</atitle><jtitle>Journal of geophysical research. Space physics</jtitle><date>2024-12</date><risdate>2024</risdate><volume>129</volume><issue>12</issue><epage>n/a</epage><issn>2169-9380</issn><eissn>2169-9402</eissn><abstract>The spatial distribution of whistler‐mode wave emissions in the Jovian magnetosphere measured during the first 45 perijove orbits of Juno is investigated. A double‐belt structure in whistler‐mode wave intensity is revealed. Between the two whistler‐mode belts, there exists a region devoid of 100 s keV electrons near the magnetic equator at 9<M<16 $9< M< 16$. Insufficient source electron population in such an electron “slot” region is a possible explanation for the relatively lower wave activity compared to the whistler‐mode belts. The wave intensity of the outer whistler‐mode belt measured in the dusk‐premidnight sector is significantly stronger than in the postmidnight‐dawn sector. We suggest that the inherent dawn‐dusk asymmetries in source electron distribution and/or auroral hiss emission rather than the modulation of solar cycle are more likely to result in the azimuthal variation of outer whistler‐mode belt intensity during the first 45 Juno perijove orbits.
Plain Language Summary
Whistler‐mode waves act as a potential driver of energetic electron dynamics in the Jovian magnetosphere. By resonating with the gyro‐bounce motion of electrons along the field line, whistler‐mode waves lead to either the acceleration of electrons or their precipitation to the atmosphere. Quantifying the net effect of such waves toward the radiation belt of Jupiter requires a comprehensive knowledge of how wavers are distributed in the Jovian magnetosphere. With NASA's Juno mission, we reveal a novel double‐belt distribution of the whistler‐mode waves. Between the inner and outer whistler‐mode belts there is a region lacking near‐equatorial energetic (100 s keV) electrons. The outer whistler‐mode belt seems to be a mixture of chorus waves generated near the equator and auroral hiss waves propagating from the polar region. Either more abundant source electrons at the duskside magnetic equator for chorus emission or stronger auroral hiss from the duskside polar region can explain the dawn‐dusk asymmetry of the outer whistler‐mode belt.
Key Points
A double‐belt structure in Jovian whistler‐mode wave (>0.1 fceq) intensity is revealed
Near‐equatorial energetic electron distributions measured by JEDI show similar radial and azimuthal profile as whistler‐mode waves
The dawn‐dusk asymmetry in the outer whistler‐mode belt intensity corresponds to either the abundance of source electrons or auroral hiss</abstract><cop>Washington</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1029/2024JA032850</doi><tpages>12</tpages><orcidid>https://orcid.org/0000-0003-4683-9533</orcidid><orcidid>https://orcid.org/0000-0002-9625-0834</orcidid><orcidid>https://orcid.org/0000-0002-9115-0789</orcidid><orcidid>https://orcid.org/0000-0002-0412-6407</orcidid><orcidid>https://orcid.org/0000-0002-5699-0678</orcidid><orcidid>https://orcid.org/0000-0001-9200-9878</orcidid><orcidid>https://orcid.org/0000-0001-6977-3472</orcidid><orcidid>https://orcid.org/0000-0002-5334-2026</orcidid><orcidid>https://orcid.org/0000-0002-0531-8814</orcidid><orcidid>https://orcid.org/0000-0003-0425-3358</orcidid><orcidid>https://orcid.org/0000-0001-6737-251X</orcidid><orcidid>https://orcid.org/0000-0002-4213-4037</orcidid><orcidid>https://orcid.org/0000-0002-4274-9760</orcidid><oa>free_for_read</oa></addata></record> |
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| ispartof | Journal of geophysical research. Space physics, 2024-12, Vol.129 (12), p.n/a |
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| source | Wiley-Blackwell Read & Publish Collection |
| subjects | Auroral hiss Chorus waves Electron distribution Electrons Emission Emission measurements Equatorial regions galileon moons Hiss Jupiter Jupiter atmosphere Jupiter probes Magnetic equator Orbits Planetary magnetospheres Polar environments Polar regions Propagation modes radiation belt Radiation belts Solar cycle Space missions Spatial distribution Wave propagation wave‐particle interaction Whistlers whistler‐mode waves |
| title | Jupiter's Whistler‐Mode Belts and Electron Slot Region |
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