Modeling of Diffuse Auroral Emission at Mars: Contribution of MeV Protons
The Solar Energetic Particle and imaging ultraviolet spectrograph (IUVS) instruments onboard the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft discovered diffuse aurora that span across the nightside of Mars due to the interaction of solar energetic particles (SEPs) with the Martian atmo...
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| Veröffentlicht in: | Journal of geophysical research. Space physics 2022-01, Vol.127 (1), p.n/a |
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| container_title | Journal of geophysical research. Space physics |
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| creator | Nakamura, Yuki Terada, Naoki Leblanc, François Rahmati, Ali Nakagawa, Hiromu Sakai, Shotaro Hiruba, Sayano Kataoka, Ryuho Murase, Kiyoka |
| description | The Solar Energetic Particle and imaging ultraviolet spectrograph (IUVS) instruments onboard the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft discovered diffuse aurora that span across the nightside of Mars due to the interaction of solar energetic particles (SEPs) with the Martian atmosphere. However, it is unclear whether the diffuse aurora originates from energetic electrons or protons. We have developed a Monte Carlo model to calculate the limb intensity profile of the CO2+ ultraviolet doublet (UVD) due to precipitation of energetic electrons and protons with energy ranges from 100 eV to 100 keV and from 50 keV to 5 MeV, respectively. We used electron and proton fluxes observed by MAVEN during the December 2014 SEP event and the September 2017 SEP event. Our results showed that proton‐induced CO2+ UVD emission has a lower peak altitude than electron‐induced CO2+ UVD emission. The calculated peak altitudes of the CO2+ UVD limb profiles are 76 and 68 km in the December 2014 event and the September 2017 event, respectively. Extending the energy to 500 keV for electrons and 20 MeV for protons further improved our comparison to the IUVS observations. We have succeeded in reproducing peak altitudes and shapes of the observed CO2+ UVD limb profiles using the SEP flux observed by MAVEN. This was possible by taking into account the contribution of energetic protons, indicating that both energetic electrons and protons contribute to producing the observed diffuse aurora.
Key Points
A Monte Carlo model was developed to investigate the contributions of precipitating electrons and protons to the diffuse auroral emission
Proton‐induced CO2+ ultraviolet doublet (UVD) emissions have lower peak altitudes than electron‐induced emissions
The Mars Atmosphere and Volatile EvolutioN/imaging ultraviolet spectrograph (IUVS) limb emission profiles of CO2+ UVD during two solar energetic particle (SEP) events were reproduced by considering the contribution of SEP protons |
| doi_str_mv | 10.1029/2021JA029914 |
| format | Article |
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Key Points
A Monte Carlo model was developed to investigate the contributions of precipitating electrons and protons to the diffuse auroral emission
Proton‐induced CO2+ ultraviolet doublet (UVD) emissions have lower peak altitudes than electron‐induced emissions
The Mars Atmosphere and Volatile EvolutioN/imaging ultraviolet spectrograph (IUVS) limb emission profiles of CO2+ UVD during two solar energetic particle (SEP) events were reproduced by considering the contribution of SEP protons</description><identifier>ISSN: 2169-9380</identifier><identifier>EISSN: 2169-9402</identifier><identifier>DOI: 10.1029/2021JA029914</identifier><language>eng</language><publisher>Washington: Blackwell Publishing Ltd</publisher><subject>Atmospheric models ; Auroral emissions ; Auroras ; Carbon dioxide ; Carbon dioxide emissions ; Cobalt ; Diffuse aurora ; Electron precipitation ; Electrons ; Emission ; Emissions ; Energetic particles ; Mars ; Mars atmosphere ; Mars missions ; Mars spacecraft ; Protons ; Sciences of the Universe ; Solar energetic particles ; Spacecraft</subject><ispartof>Journal of geophysical research. Space physics, 2022-01, Vol.127 (1), p.n/a</ispartof><rights>2022. American Geophysical Union. All Rights Reserved.</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c4461-dd1aec41f71b5b2f1c95c487aa93773a332e11cce6fb2a83c4b75459588603a63</citedby><cites>FETCH-LOGICAL-c4461-dd1aec41f71b5b2f1c95c487aa93773a332e11cce6fb2a83c4b75459588603a63</cites><orcidid>0000-0001-9400-1765 ; 0000-0003-1700-238X ; 0000-0003-0519-6498 ; 0000-0001-9135-2076 ; 0000-0001-5685-9736 ; 0000-0001-8166-0171 ; 0000-0001-8871-9199 ; 0000-0002-5548-3519 ; 0000-0001-8851-9146</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%2F2021JA029914$$EPDF$$P50$$Gwiley$$H</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1029%2F2021JA029914$$EHTML$$P50$$Gwiley$$H</linktohtml><link.rule.ids>230,314,776,780,881,1411,1427,4009,27902,27903,27904,45553,45554,46387,46811</link.rule.ids><backlink>$$Uhttps://insu.hal.science/insu-03517910$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Nakamura, Yuki</creatorcontrib><creatorcontrib>Terada, Naoki</creatorcontrib><creatorcontrib>Leblanc, François</creatorcontrib><creatorcontrib>Rahmati, Ali</creatorcontrib><creatorcontrib>Nakagawa, Hiromu</creatorcontrib><creatorcontrib>Sakai, Shotaro</creatorcontrib><creatorcontrib>Hiruba, Sayano</creatorcontrib><creatorcontrib>Kataoka, Ryuho</creatorcontrib><creatorcontrib>Murase, Kiyoka</creatorcontrib><title>Modeling of Diffuse Auroral Emission at Mars: Contribution of MeV Protons</title><title>Journal of geophysical research. Space physics</title><description>The Solar Energetic Particle and imaging ultraviolet spectrograph (IUVS) instruments onboard the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft discovered diffuse aurora that span across the nightside of Mars due to the interaction of solar energetic particles (SEPs) with the Martian atmosphere. However, it is unclear whether the diffuse aurora originates from energetic electrons or protons. We have developed a Monte Carlo model to calculate the limb intensity profile of the CO2+ ultraviolet doublet (UVD) due to precipitation of energetic electrons and protons with energy ranges from 100 eV to 100 keV and from 50 keV to 5 MeV, respectively. We used electron and proton fluxes observed by MAVEN during the December 2014 SEP event and the September 2017 SEP event. Our results showed that proton‐induced CO2+ UVD emission has a lower peak altitude than electron‐induced CO2+ UVD emission. The calculated peak altitudes of the CO2+ UVD limb profiles are 76 and 68 km in the December 2014 event and the September 2017 event, respectively. Extending the energy to 500 keV for electrons and 20 MeV for protons further improved our comparison to the IUVS observations. We have succeeded in reproducing peak altitudes and shapes of the observed CO2+ UVD limb profiles using the SEP flux observed by MAVEN. This was possible by taking into account the contribution of energetic protons, indicating that both energetic electrons and protons contribute to producing the observed diffuse aurora.
Key Points
A Monte Carlo model was developed to investigate the contributions of precipitating electrons and protons to the diffuse auroral emission
Proton‐induced CO2+ ultraviolet doublet (UVD) emissions have lower peak altitudes than electron‐induced emissions
The Mars Atmosphere and Volatile EvolutioN/imaging ultraviolet spectrograph (IUVS) limb emission profiles of CO2+ UVD during two solar energetic particle (SEP) events were reproduced by considering the contribution of SEP protons</description><subject>Atmospheric models</subject><subject>Auroral emissions</subject><subject>Auroras</subject><subject>Carbon dioxide</subject><subject>Carbon dioxide emissions</subject><subject>Cobalt</subject><subject>Diffuse aurora</subject><subject>Electron precipitation</subject><subject>Electrons</subject><subject>Emission</subject><subject>Emissions</subject><subject>Energetic particles</subject><subject>Mars</subject><subject>Mars atmosphere</subject><subject>Mars missions</subject><subject>Mars spacecraft</subject><subject>Protons</subject><subject>Sciences of the Universe</subject><subject>Solar energetic particles</subject><subject>Spacecraft</subject><issn>2169-9380</issn><issn>2169-9402</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><recordid>eNp9kN1LwzAUxYsoOHRv_gEB38Rqbj7axrcy5z7YUER9DWmXakbXzKRV9t-bURWfvC_3cPjdw-VE0RngK8BEXBNMYJ4HJYAdRAMCiYgFw-TwR9MMH0dD79c4TBYs4INotrQrXZvmFdkK3Zqq6rxGeeesUzUab4z3xjZItWipnL9BI9u0zhRdu3fDxVK_oAdnW9v40-ioUrXXw-99Ej3fjZ9G03hxP5mN8kVcMpZAvFqB0iWDKoWCF6SCUvCSZalSgqYpVZQSDVCWOqkKojJasiLljAueZQmmKqEn0UWf-6ZquXVmo9xOWmXkNF9I0_hOYsohFYA_IMDnPbx19r3TvpVr27km_CdJQlioIGMiUJc9VTrrvdPVby5guS9X_i034LTHP02td_-ycj55zHkiUqBfQO54Cg</recordid><startdate>202201</startdate><enddate>202201</enddate><creator>Nakamura, Yuki</creator><creator>Terada, Naoki</creator><creator>Leblanc, François</creator><creator>Rahmati, Ali</creator><creator>Nakagawa, Hiromu</creator><creator>Sakai, Shotaro</creator><creator>Hiruba, Sayano</creator><creator>Kataoka, Ryuho</creator><creator>Murase, Kiyoka</creator><general>Blackwell Publishing Ltd</general><general>American Geophysical Union/Wiley</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>1XC</scope><scope>VOOES</scope><orcidid>https://orcid.org/0000-0001-9400-1765</orcidid><orcidid>https://orcid.org/0000-0003-1700-238X</orcidid><orcidid>https://orcid.org/0000-0003-0519-6498</orcidid><orcidid>https://orcid.org/0000-0001-9135-2076</orcidid><orcidid>https://orcid.org/0000-0001-5685-9736</orcidid><orcidid>https://orcid.org/0000-0001-8166-0171</orcidid><orcidid>https://orcid.org/0000-0001-8871-9199</orcidid><orcidid>https://orcid.org/0000-0002-5548-3519</orcidid><orcidid>https://orcid.org/0000-0001-8851-9146</orcidid></search><sort><creationdate>202201</creationdate><title>Modeling of Diffuse Auroral Emission at Mars: Contribution of MeV Protons</title><author>Nakamura, Yuki ; Terada, Naoki ; Leblanc, François ; Rahmati, Ali ; Nakagawa, Hiromu ; Sakai, Shotaro ; Hiruba, Sayano ; Kataoka, Ryuho ; Murase, Kiyoka</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c4461-dd1aec41f71b5b2f1c95c487aa93773a332e11cce6fb2a83c4b75459588603a63</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Atmospheric models</topic><topic>Auroral emissions</topic><topic>Auroras</topic><topic>Carbon dioxide</topic><topic>Carbon dioxide emissions</topic><topic>Cobalt</topic><topic>Diffuse aurora</topic><topic>Electron precipitation</topic><topic>Electrons</topic><topic>Emission</topic><topic>Emissions</topic><topic>Energetic particles</topic><topic>Mars</topic><topic>Mars atmosphere</topic><topic>Mars missions</topic><topic>Mars spacecraft</topic><topic>Protons</topic><topic>Sciences of the Universe</topic><topic>Solar energetic particles</topic><topic>Spacecraft</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Nakamura, Yuki</creatorcontrib><creatorcontrib>Terada, Naoki</creatorcontrib><creatorcontrib>Leblanc, François</creatorcontrib><creatorcontrib>Rahmati, Ali</creatorcontrib><creatorcontrib>Nakagawa, Hiromu</creatorcontrib><creatorcontrib>Sakai, Shotaro</creatorcontrib><creatorcontrib>Hiruba, Sayano</creatorcontrib><creatorcontrib>Kataoka, Ryuho</creatorcontrib><creatorcontrib>Murase, Kiyoka</creatorcontrib><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>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><jtitle>Journal of geophysical research. Space physics</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Nakamura, Yuki</au><au>Terada, Naoki</au><au>Leblanc, François</au><au>Rahmati, Ali</au><au>Nakagawa, Hiromu</au><au>Sakai, Shotaro</au><au>Hiruba, Sayano</au><au>Kataoka, Ryuho</au><au>Murase, Kiyoka</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Modeling of Diffuse Auroral Emission at Mars: Contribution of MeV Protons</atitle><jtitle>Journal of geophysical research. Space physics</jtitle><date>2022-01</date><risdate>2022</risdate><volume>127</volume><issue>1</issue><epage>n/a</epage><issn>2169-9380</issn><eissn>2169-9402</eissn><abstract>The Solar Energetic Particle and imaging ultraviolet spectrograph (IUVS) instruments onboard the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft discovered diffuse aurora that span across the nightside of Mars due to the interaction of solar energetic particles (SEPs) with the Martian atmosphere. However, it is unclear whether the diffuse aurora originates from energetic electrons or protons. We have developed a Monte Carlo model to calculate the limb intensity profile of the CO2+ ultraviolet doublet (UVD) due to precipitation of energetic electrons and protons with energy ranges from 100 eV to 100 keV and from 50 keV to 5 MeV, respectively. We used electron and proton fluxes observed by MAVEN during the December 2014 SEP event and the September 2017 SEP event. Our results showed that proton‐induced CO2+ UVD emission has a lower peak altitude than electron‐induced CO2+ UVD emission. The calculated peak altitudes of the CO2+ UVD limb profiles are 76 and 68 km in the December 2014 event and the September 2017 event, respectively. Extending the energy to 500 keV for electrons and 20 MeV for protons further improved our comparison to the IUVS observations. We have succeeded in reproducing peak altitudes and shapes of the observed CO2+ UVD limb profiles using the SEP flux observed by MAVEN. This was possible by taking into account the contribution of energetic protons, indicating that both energetic electrons and protons contribute to producing the observed diffuse aurora.
Key Points
A Monte Carlo model was developed to investigate the contributions of precipitating electrons and protons to the diffuse auroral emission
Proton‐induced CO2+ ultraviolet doublet (UVD) emissions have lower peak altitudes than electron‐induced emissions
The Mars Atmosphere and Volatile EvolutioN/imaging ultraviolet spectrograph (IUVS) limb emission profiles of CO2+ UVD during two solar energetic particle (SEP) events were reproduced by considering the contribution of SEP protons</abstract><cop>Washington</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1029/2021JA029914</doi><tpages>19</tpages><orcidid>https://orcid.org/0000-0001-9400-1765</orcidid><orcidid>https://orcid.org/0000-0003-1700-238X</orcidid><orcidid>https://orcid.org/0000-0003-0519-6498</orcidid><orcidid>https://orcid.org/0000-0001-9135-2076</orcidid><orcidid>https://orcid.org/0000-0001-5685-9736</orcidid><orcidid>https://orcid.org/0000-0001-8166-0171</orcidid><orcidid>https://orcid.org/0000-0001-8871-9199</orcidid><orcidid>https://orcid.org/0000-0002-5548-3519</orcidid><orcidid>https://orcid.org/0000-0001-8851-9146</orcidid><oa>free_for_read</oa></addata></record> |
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| subjects | Atmospheric models Auroral emissions Auroras Carbon dioxide Carbon dioxide emissions Cobalt Diffuse aurora Electron precipitation Electrons Emission Emissions Energetic particles Mars Mars atmosphere Mars missions Mars spacecraft Protons Sciences of the Universe Solar energetic particles Spacecraft |
| title | Modeling of Diffuse Auroral Emission at Mars: Contribution of MeV Protons |
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