Proton cyclotron waves occurrence rate upstream from Mars observed by MAVEN: Associated variability of the Martian upper atmosphere
Measurements provided by the Magnetometer and the Extreme Ultraviolet Monitor (EUVM) on board the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft together with atomic H exospheric densities derived from numerical simulations are studied for the time interval from October 2014 up to March 2...
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| Veröffentlicht in: | Journal of geophysical research. Space physics 2016-11, Vol.121 (11), p.11,113-11,128 |
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| creator | Romanelli, N. Mazelle, C. Chaufray, J. Y. Meziane, K. Shan, L. Ruhunusiri, S. Connerney, J. E. P. Espley, J. R. Eparvier, F. Thiemann, E. Halekas, J. S. Mitchell, D. L. McFadden, J. P. Brain, D. Jakosky, B. M. |
| description | Measurements provided by the Magnetometer and the Extreme Ultraviolet Monitor (EUVM) on board the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft together with atomic H exospheric densities derived from numerical simulations are studied for the time interval from October 2014 up to March 2016. We determine the proton cyclotron waves (PCWs) occurrence rate observed upstream from Mars at different times. We also study the relationship with temporal variabilities of the high‐altitude Martian hydrogen exosphere and the solar EUV flux reaching the Martian environment. We find that the abundance of PCWs is higher when Mars is close to perihelion and decreases to lower and approximately constant values after the Martian Northern Spring Equinox. We also conclude that these variabilities cannot be associated with biases in MAVEN's spatial coverage or changes in the background magnetic field orientation. Higher H exospheric densities on the Martian dayside are also found when Mars is closer to perihelion, as a result of changes in the thermospheric response to variability in the ultraviolet flux reaching Mars at different orbital distances. A consistent behavior is also observed in the analyzed daily irradiances measured by the MAVEN EUVM. The latter trends point toward an increase in the planetary proton densities upstream from the Martian bow shock near perihelion. These results then suggest a method to indirectly monitor the variability of the H exosphere up to very high altitudes during large time intervals (compared to direct measurements of neutral particles), based on the observed abundance of PCWs.
Key Points
First confirmation that PCWs abundance upstream from the Martian bow shock varies with time, with higher values near perihelion
At higher altitudes, temporal variabilities in the dayside exospheric H density display a similar long‐term trend
Exospheric variability partly caused by solar UV forcing on the thermosphere; water vapor might also contribute |
| doi_str_mv | 10.1002/2016JA023270 |
| format | Article |
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Key Points
First confirmation that PCWs abundance upstream from the Martian bow shock varies with time, with higher values near perihelion
At higher altitudes, temporal variabilities in the dayside exospheric H density display a similar long‐term trend
Exospheric variability partly caused by solar UV forcing on the thermosphere; water vapor might also contribute</description><identifier>ISSN: 2169-9380</identifier><identifier>EISSN: 2169-9402</identifier><identifier>DOI: 10.1002/2016JA023270</identifier><language>eng</language><publisher>Washington: Blackwell Publishing Ltd</publisher><subject>Abundance ; Altitude ; Astrophysics ; Atmosphere ; Computer simulation ; Cyclotrons ; Density ; Earth and Planetary Astrophysics ; EUV flux ; Evolution ; Exosphere ; Extreme ultraviolet radiation ; Flux ; H exosphere ; High altitude ; Hydrogen ; Irradiance ; Magnetic fields ; Mars ; Mars (planet) ; Mars atmosphere ; Mars missions ; Mars spacecraft ; Monitors ; Neutral particles ; Numerical simulations ; Onboard ; Particle physics ; PCWs ; Perihelions ; Planetary magnetic fields ; Sciences of the Universe ; Solar and Stellar Astrophysics ; Solar EUV ; Spacecraft ; temporal variability ; Thermosphere ; Upper atmosphere ; Upstream ; Water vapor</subject><ispartof>Journal of geophysical research. Space physics, 2016-11, Vol.121 (11), p.11,113-11,128</ispartof><rights>2016. 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-c6809-af420e94ae1adc779be926edebc1b83c64c36d8426f12ef5dda2000bead975313</citedby><cites>FETCH-LOGICAL-c6809-af420e94ae1adc779be926edebc1b83c64c36d8426f12ef5dda2000bead975313</cites><orcidid>0000-0002-7613-8749 ; 0000-0002-2354-9261 ; 0000-0002-5305-9466 ; 0000-0002-4089-0234 ; 0000-0002-0758-9976 ; 0000-0001-9210-0284 ; 0000-0001-5258-6128 ; 0000-0001-8932-368X ; 0000-0001-7143-2730 ; 0000-0001-9154-7236 ; 0000-0002-2527-9816 ; 0000-0002-6371-9683</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://onlinelibrary.wiley.com/doi/pdf/10.1002%2F2016JA023270$$EPDF$$P50$$Gwiley$$H</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1002%2F2016JA023270$$EHTML$$P50$$Gwiley$$H</linktohtml><link.rule.ids>230,314,777,781,882,1412,1428,27905,27906,45555,45556,46390,46814</link.rule.ids><backlink>$$Uhttps://insu.hal.science/insu-01397677$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Romanelli, N.</creatorcontrib><creatorcontrib>Mazelle, C.</creatorcontrib><creatorcontrib>Chaufray, J. Y.</creatorcontrib><creatorcontrib>Meziane, K.</creatorcontrib><creatorcontrib>Shan, L.</creatorcontrib><creatorcontrib>Ruhunusiri, S.</creatorcontrib><creatorcontrib>Connerney, J. E. P.</creatorcontrib><creatorcontrib>Espley, J. R.</creatorcontrib><creatorcontrib>Eparvier, F.</creatorcontrib><creatorcontrib>Thiemann, E.</creatorcontrib><creatorcontrib>Halekas, J. S.</creatorcontrib><creatorcontrib>Mitchell, D. L.</creatorcontrib><creatorcontrib>McFadden, J. P.</creatorcontrib><creatorcontrib>Brain, D.</creatorcontrib><creatorcontrib>Jakosky, B. M.</creatorcontrib><title>Proton cyclotron waves occurrence rate upstream from Mars observed by MAVEN: Associated variability of the Martian upper atmosphere</title><title>Journal of geophysical research. Space physics</title><description>Measurements provided by the Magnetometer and the Extreme Ultraviolet Monitor (EUVM) on board the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft together with atomic H exospheric densities derived from numerical simulations are studied for the time interval from October 2014 up to March 2016. We determine the proton cyclotron waves (PCWs) occurrence rate observed upstream from Mars at different times. We also study the relationship with temporal variabilities of the high‐altitude Martian hydrogen exosphere and the solar EUV flux reaching the Martian environment. We find that the abundance of PCWs is higher when Mars is close to perihelion and decreases to lower and approximately constant values after the Martian Northern Spring Equinox. We also conclude that these variabilities cannot be associated with biases in MAVEN's spatial coverage or changes in the background magnetic field orientation. Higher H exospheric densities on the Martian dayside are also found when Mars is closer to perihelion, as a result of changes in the thermospheric response to variability in the ultraviolet flux reaching Mars at different orbital distances. A consistent behavior is also observed in the analyzed daily irradiances measured by the MAVEN EUVM. The latter trends point toward an increase in the planetary proton densities upstream from the Martian bow shock near perihelion. These results then suggest a method to indirectly monitor the variability of the H exosphere up to very high altitudes during large time intervals (compared to direct measurements of neutral particles), based on the observed abundance of PCWs.
Key Points
First confirmation that PCWs abundance upstream from the Martian bow shock varies with time, with higher values near perihelion
At higher altitudes, temporal variabilities in the dayside exospheric H density display a similar long‐term trend
Exospheric variability partly caused by solar UV forcing on the thermosphere; water vapor might also contribute</description><subject>Abundance</subject><subject>Altitude</subject><subject>Astrophysics</subject><subject>Atmosphere</subject><subject>Computer simulation</subject><subject>Cyclotrons</subject><subject>Density</subject><subject>Earth and Planetary Astrophysics</subject><subject>EUV flux</subject><subject>Evolution</subject><subject>Exosphere</subject><subject>Extreme ultraviolet radiation</subject><subject>Flux</subject><subject>H exosphere</subject><subject>High altitude</subject><subject>Hydrogen</subject><subject>Irradiance</subject><subject>Magnetic fields</subject><subject>Mars</subject><subject>Mars (planet)</subject><subject>Mars atmosphere</subject><subject>Mars missions</subject><subject>Mars spacecraft</subject><subject>Monitors</subject><subject>Neutral particles</subject><subject>Numerical simulations</subject><subject>Onboard</subject><subject>Particle physics</subject><subject>PCWs</subject><subject>Perihelions</subject><subject>Planetary magnetic fields</subject><subject>Sciences of the Universe</subject><subject>Solar and Stellar Astrophysics</subject><subject>Solar EUV</subject><subject>Spacecraft</subject><subject>temporal variability</subject><subject>Thermosphere</subject><subject>Upper atmosphere</subject><subject>Upstream</subject><subject>Water vapor</subject><issn>2169-9380</issn><issn>2169-9402</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2016</creationdate><recordtype>article</recordtype><recordid>eNqN0kuL1TAUB_AiCg7j7PwAATciXs2rebgrwzwc7qiIug1pesrN0DY1Se_QtV_cXK6KuBjMJofwy4H_4VTVc4LfEIzpW4qJuGkwZVTiR9UJJUJvNMf08e-aKfy0OkvpDpejyhOpT6ofn2LIYUJudUPIsVT3dg8JBeeWGGFygKLNgJY55Qh2RH0MI7q1sZA2QdxDh9oV3TbfLj68Q01KwfniO7S30dvWDz6vKPQo7-DwK3s7lV4zRGTzGNK8gwjPqie9HRKc_bpPq6-XF1_Orzfbj1fvz5vtxgmF9cb2nGLQ3AKxnZNSt6CpgA5aR1rFnOCOiU5xKnpCoa-7ztKStAXbaVkzwk6rV8e-OzuYOfrRxtUE6811szV-SovBhGkppNwf8MsjnmP4vkDKZvTJwTDYCcKSDFGqTF0xwf-D1pprJWtc6It_6F1Y4lRSG6JprQmVRD2oFNecMyJFUa-PysWQUoT-TyaCzWElzN8rUTg78ns_wPqgNTdXn5uaYa3ZT_potqg</recordid><startdate>201611</startdate><enddate>201611</enddate><creator>Romanelli, N.</creator><creator>Mazelle, C.</creator><creator>Chaufray, J. Y.</creator><creator>Meziane, K.</creator><creator>Shan, L.</creator><creator>Ruhunusiri, S.</creator><creator>Connerney, J. E. P.</creator><creator>Espley, J. R.</creator><creator>Eparvier, F.</creator><creator>Thiemann, E.</creator><creator>Halekas, J. S.</creator><creator>Mitchell, D. L.</creator><creator>McFadden, J. P.</creator><creator>Brain, D.</creator><creator>Jakosky, B. M.</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/0000-0002-7613-8749</orcidid><orcidid>https://orcid.org/0000-0002-2354-9261</orcidid><orcidid>https://orcid.org/0000-0002-5305-9466</orcidid><orcidid>https://orcid.org/0000-0002-4089-0234</orcidid><orcidid>https://orcid.org/0000-0002-0758-9976</orcidid><orcidid>https://orcid.org/0000-0001-9210-0284</orcidid><orcidid>https://orcid.org/0000-0001-5258-6128</orcidid><orcidid>https://orcid.org/0000-0001-8932-368X</orcidid><orcidid>https://orcid.org/0000-0001-7143-2730</orcidid><orcidid>https://orcid.org/0000-0001-9154-7236</orcidid><orcidid>https://orcid.org/0000-0002-2527-9816</orcidid><orcidid>https://orcid.org/0000-0002-6371-9683</orcidid></search><sort><creationdate>201611</creationdate><title>Proton cyclotron waves occurrence rate upstream from Mars observed by MAVEN: Associated variability of the Martian upper atmosphere</title><author>Romanelli, N. ; Mazelle, C. ; Chaufray, J. Y. ; Meziane, K. ; Shan, L. ; Ruhunusiri, S. ; Connerney, J. E. P. ; Espley, J. R. ; Eparvier, F. ; Thiemann, E. ; Halekas, J. S. ; Mitchell, D. L. ; McFadden, J. P. ; Brain, D. ; Jakosky, B. M.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c6809-af420e94ae1adc779be926edebc1b83c64c36d8426f12ef5dda2000bead975313</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2016</creationdate><topic>Abundance</topic><topic>Altitude</topic><topic>Astrophysics</topic><topic>Atmosphere</topic><topic>Computer simulation</topic><topic>Cyclotrons</topic><topic>Density</topic><topic>Earth and Planetary Astrophysics</topic><topic>EUV flux</topic><topic>Evolution</topic><topic>Exosphere</topic><topic>Extreme ultraviolet radiation</topic><topic>Flux</topic><topic>H exosphere</topic><topic>High altitude</topic><topic>Hydrogen</topic><topic>Irradiance</topic><topic>Magnetic fields</topic><topic>Mars</topic><topic>Mars (planet)</topic><topic>Mars atmosphere</topic><topic>Mars missions</topic><topic>Mars spacecraft</topic><topic>Monitors</topic><topic>Neutral particles</topic><topic>Numerical simulations</topic><topic>Onboard</topic><topic>Particle physics</topic><topic>PCWs</topic><topic>Perihelions</topic><topic>Planetary magnetic fields</topic><topic>Sciences of the Universe</topic><topic>Solar and Stellar Astrophysics</topic><topic>Solar EUV</topic><topic>Spacecraft</topic><topic>temporal variability</topic><topic>Thermosphere</topic><topic>Upper atmosphere</topic><topic>Upstream</topic><topic>Water vapor</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Romanelli, N.</creatorcontrib><creatorcontrib>Mazelle, C.</creatorcontrib><creatorcontrib>Chaufray, J. Y.</creatorcontrib><creatorcontrib>Meziane, K.</creatorcontrib><creatorcontrib>Shan, L.</creatorcontrib><creatorcontrib>Ruhunusiri, S.</creatorcontrib><creatorcontrib>Connerney, J. E. P.</creatorcontrib><creatorcontrib>Espley, J. R.</creatorcontrib><creatorcontrib>Eparvier, F.</creatorcontrib><creatorcontrib>Thiemann, E.</creatorcontrib><creatorcontrib>Halekas, J. S.</creatorcontrib><creatorcontrib>Mitchell, D. L.</creatorcontrib><creatorcontrib>McFadden, J. P.</creatorcontrib><creatorcontrib>Brain, D.</creatorcontrib><creatorcontrib>Jakosky, B. M.</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>Romanelli, N.</au><au>Mazelle, C.</au><au>Chaufray, J. Y.</au><au>Meziane, K.</au><au>Shan, L.</au><au>Ruhunusiri, S.</au><au>Connerney, J. E. P.</au><au>Espley, J. R.</au><au>Eparvier, F.</au><au>Thiemann, E.</au><au>Halekas, J. S.</au><au>Mitchell, D. L.</au><au>McFadden, J. P.</au><au>Brain, D.</au><au>Jakosky, B. M.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Proton cyclotron waves occurrence rate upstream from Mars observed by MAVEN: Associated variability of the Martian upper atmosphere</atitle><jtitle>Journal of geophysical research. Space physics</jtitle><date>2016-11</date><risdate>2016</risdate><volume>121</volume><issue>11</issue><spage>11,113</spage><epage>11,128</epage><pages>11,113-11,128</pages><issn>2169-9380</issn><eissn>2169-9402</eissn><abstract>Measurements provided by the Magnetometer and the Extreme Ultraviolet Monitor (EUVM) on board the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft together with atomic H exospheric densities derived from numerical simulations are studied for the time interval from October 2014 up to March 2016. We determine the proton cyclotron waves (PCWs) occurrence rate observed upstream from Mars at different times. We also study the relationship with temporal variabilities of the high‐altitude Martian hydrogen exosphere and the solar EUV flux reaching the Martian environment. We find that the abundance of PCWs is higher when Mars is close to perihelion and decreases to lower and approximately constant values after the Martian Northern Spring Equinox. We also conclude that these variabilities cannot be associated with biases in MAVEN's spatial coverage or changes in the background magnetic field orientation. Higher H exospheric densities on the Martian dayside are also found when Mars is closer to perihelion, as a result of changes in the thermospheric response to variability in the ultraviolet flux reaching Mars at different orbital distances. A consistent behavior is also observed in the analyzed daily irradiances measured by the MAVEN EUVM. The latter trends point toward an increase in the planetary proton densities upstream from the Martian bow shock near perihelion. These results then suggest a method to indirectly monitor the variability of the H exosphere up to very high altitudes during large time intervals (compared to direct measurements of neutral particles), based on the observed abundance of PCWs.
Key Points
First confirmation that PCWs abundance upstream from the Martian bow shock varies with time, with higher values near perihelion
At higher altitudes, temporal variabilities in the dayside exospheric H density display a similar long‐term trend
Exospheric variability partly caused by solar UV forcing on the thermosphere; water vapor might also contribute</abstract><cop>Washington</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1002/2016JA023270</doi><tpages>16</tpages><orcidid>https://orcid.org/0000-0002-7613-8749</orcidid><orcidid>https://orcid.org/0000-0002-2354-9261</orcidid><orcidid>https://orcid.org/0000-0002-5305-9466</orcidid><orcidid>https://orcid.org/0000-0002-4089-0234</orcidid><orcidid>https://orcid.org/0000-0002-0758-9976</orcidid><orcidid>https://orcid.org/0000-0001-9210-0284</orcidid><orcidid>https://orcid.org/0000-0001-5258-6128</orcidid><orcidid>https://orcid.org/0000-0001-8932-368X</orcidid><orcidid>https://orcid.org/0000-0001-7143-2730</orcidid><orcidid>https://orcid.org/0000-0001-9154-7236</orcidid><orcidid>https://orcid.org/0000-0002-2527-9816</orcidid><orcidid>https://orcid.org/0000-0002-6371-9683</orcidid><oa>free_for_read</oa></addata></record> |
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| ispartof | Journal of geophysical research. Space physics, 2016-11, Vol.121 (11), p.11,113-11,128 |
| issn | 2169-9380 2169-9402 |
| language | eng |
| recordid | cdi_hal_primary_oai_HAL_insu_01397677v1 |
| source | Wiley Online Library Journals Frontfile Complete; Wiley Free Content |
| subjects | Abundance Altitude Astrophysics Atmosphere Computer simulation Cyclotrons Density Earth and Planetary Astrophysics EUV flux Evolution Exosphere Extreme ultraviolet radiation Flux H exosphere High altitude Hydrogen Irradiance Magnetic fields Mars Mars (planet) Mars atmosphere Mars missions Mars spacecraft Monitors Neutral particles Numerical simulations Onboard Particle physics PCWs Perihelions Planetary magnetic fields Sciences of the Universe Solar and Stellar Astrophysics Solar EUV Spacecraft temporal variability Thermosphere Upper atmosphere Upstream Water vapor |
| title | Proton cyclotron waves occurrence rate upstream from Mars observed by MAVEN: Associated variability of the Martian upper atmosphere |
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