Oxygen and hydrogen ion abundance in the near-Earth magnetosphere: Statistical results on the response to the geomagnetic and solar wind activity conditions
The composition of ions plays a crucial role for the fundamental plasma properties in the terrestrial magnetosphere. We investigate the oxygen‐to‐hydrogen ratio in the near‐Earth magnetosphere from −10 RE 274 keV O+ ion intensities, relative to the corresponding hydrogen intensities; (3) In contrast...
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| Veröffentlicht in: | Journal of Geophysical Research: Space Physics 2012-12, Vol.117 (A12), p.n/a |
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| container_title | Journal of Geophysical Research: Space Physics |
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| creator | Kronberg, E. A. Haaland, S. E. Daly, P. W. Grigorenko, E. E. Kistler, L. M. Fränz, M. Dandouras, I. |
| description | The composition of ions plays a crucial role for the fundamental plasma properties in the terrestrial magnetosphere. We investigate the oxygen‐to‐hydrogen ratio in the near‐Earth magnetosphere from −10 RE 274 keV O+ ion intensities, relative to the corresponding hydrogen intensities; (3) In contrast to ∼10 keV ions, the >274 keV O+ions show the strongest acceleration during growth phase and not during the expansion phase itself. This suggests a connection between the energy input to the magnetosphere and the effective energization of energetic ions during growth phase; (4) The ratio between quiet and disturbed times for the intensities of ion ionospheric outflow is similar to those observed in the near‐Earth magnetosphere at >274 keV. Therefore, the increase of the energetic ion intensity during disturbed time is likely due to the intensification and the effective acceleration of the ionospheric source. In conclusion, the energization process in the near‐Earth magnetosphere is mass dependent and it is more effective for the heavier ions.
Key Points
Response of the O+ and H+ to the geomagnetic and solar wind changes
The strongest energetic O+ acceleration is during growth phase
O+ at lower energies is strongly affected by storms and substorms |
| doi_str_mv | 10.1029/2012JA018071 |
| format | Article |
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Key Points
Response of the O+ and H+ to the geomagnetic and solar wind changes
The strongest energetic O+ acceleration is during growth phase
O+ at lower energies is strongly affected by storms and substorms</description><identifier>ISSN: 0148-0227</identifier><identifier>ISSN: 2169-9380</identifier><identifier>EISSN: 2156-2202</identifier><identifier>EISSN: 2169-9402</identifier><identifier>DOI: 10.1029/2012JA018071</identifier><language>eng</language><publisher>Washington: Blackwell Publishing Ltd</publisher><subject>Atmospheric sciences ; Earth ; Hydrogen ions ; Magnetic fields ; Magnetism ; oxygen abundance ; Plasma physics ; response to solar wind ; Space ; storm ; substorms</subject><ispartof>Journal of Geophysical Research: Space Physics, 2012-12, Vol.117 (A12), p.n/a</ispartof><rights>2012 by the American Geophysical Union</rights><rights>Copyright American Geophysical Union 2012</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c4493-21d5c1ec86955bc3379ce57163cba6953a48073551a47f22e869d5c90717ce683</citedby><cites>FETCH-LOGICAL-c4493-21d5c1ec86955bc3379ce57163cba6953a48073551a47f22e869d5c90717ce683</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://onlinelibrary.wiley.com/doi/pdf/10.1029%2F2012JA018071$$EPDF$$P50$$Gwiley$$H</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1029%2F2012JA018071$$EHTML$$P50$$Gwiley$$H</linktohtml><link.rule.ids>314,776,780,1411,1427,11494,27903,27904,45553,45554,46387,46446,46811,46870</link.rule.ids></links><search><creatorcontrib>Kronberg, E. A.</creatorcontrib><creatorcontrib>Haaland, S. E.</creatorcontrib><creatorcontrib>Daly, P. W.</creatorcontrib><creatorcontrib>Grigorenko, E. E.</creatorcontrib><creatorcontrib>Kistler, L. M.</creatorcontrib><creatorcontrib>Fränz, M.</creatorcontrib><creatorcontrib>Dandouras, I.</creatorcontrib><title>Oxygen and hydrogen ion abundance in the near-Earth magnetosphere: Statistical results on the response to the geomagnetic and solar wind activity conditions</title><title>Journal of Geophysical Research: Space Physics</title><addtitle>J. Geophys. Res</addtitle><description>The composition of ions plays a crucial role for the fundamental plasma properties in the terrestrial magnetosphere. We investigate the oxygen‐to‐hydrogen ratio in the near‐Earth magnetosphere from −10 RE < XGSE < 10 RE. The results are based on seven years of ion flux measurements in the energy range ∼10 keV to ∼955 keV from the RAPID and CIS instruments on board the Cluster satellites. We find that (1) hydrogen ions at ∼10 keV show only a slight correlation with the geomagnetic conditions and interplanetary magnetic field changes. They are best correlated with the solar wind dynamic pressure and density, which is an expected effect of the magnetospheric compression; (2) ∼10 keV O+ ion intensities are more strongly affected during disturbed phase of a geomagnetic storm or substorm than >274 keV O+ ion intensities, relative to the corresponding hydrogen intensities; (3) In contrast to ∼10 keV ions, the >274 keV O+ions show the strongest acceleration during growth phase and not during the expansion phase itself. This suggests a connection between the energy input to the magnetosphere and the effective energization of energetic ions during growth phase; (4) The ratio between quiet and disturbed times for the intensities of ion ionospheric outflow is similar to those observed in the near‐Earth magnetosphere at >274 keV. Therefore, the increase of the energetic ion intensity during disturbed time is likely due to the intensification and the effective acceleration of the ionospheric source. In conclusion, the energization process in the near‐Earth magnetosphere is mass dependent and it is more effective for the heavier ions.
Key Points
Response of the O+ and H+ to the geomagnetic and solar wind changes
The strongest energetic O+ acceleration is during growth phase
O+ at lower energies is strongly affected by storms and substorms</description><subject>Atmospheric sciences</subject><subject>Earth</subject><subject>Hydrogen ions</subject><subject>Magnetic fields</subject><subject>Magnetism</subject><subject>oxygen abundance</subject><subject>Plasma physics</subject><subject>response to solar wind</subject><subject>Space</subject><subject>storm</subject><subject>substorms</subject><issn>0148-0227</issn><issn>2169-9380</issn><issn>2156-2202</issn><issn>2169-9402</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2012</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GNUQQ</sourceid><recordid>eNp9kd1uEzEQhS0EElHpHQ9gidsu-Hed5S5qS6CqqMSPQNxYjneSuGzt1HZI9114WKZdVHGFb8ZndD6PdYaQl5y95kx0bwTj4mLB-JwZ_oTMBNdtIwQTT8mMcTVvmBDmOTku5ZrhUbpVjM_I76u7cQORutjT7djndC9CwsZqH3sXPdAQad0CjeByc-5y3dIbt4lQU9ltIcNb-rm6GkoN3g00Q9kPtdA0QSh3KRagNT3oDaQJDv5hZEmDy_QQ8Op8Db9CHalPsQ8V_1BekGdrNxQ4_luPyNd3519O3zeXV8sPp4vLxivVyUbwXnsOft52Wq-8lKbzoA1vpV857EmnMBSpNXfKrIUANCLRYVDGQzuXR-TV9O4up9s9lGqv0z5HHGm5kIYzg3Gh62Ry-ZxKybC2uxxuXB4tZ_Z-BfbfFaBdTvZDGGD8r9deLD8thBBKItVMFAYKd4-Uyz9ta6TR9tvHpT37cYaFfbdK_gGYUZg9</recordid><startdate>201212</startdate><enddate>201212</enddate><creator>Kronberg, E. A.</creator><creator>Haaland, S. E.</creator><creator>Daly, P. W.</creator><creator>Grigorenko, E. E.</creator><creator>Kistler, L. M.</creator><creator>Fränz, M.</creator><creator>Dandouras, I.</creator><general>Blackwell Publishing Ltd</general><scope>BSCLL</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>3V.</scope><scope>7TG</scope><scope>7XB</scope><scope>88I</scope><scope>8FD</scope><scope>8FE</scope><scope>8FG</scope><scope>8FK</scope><scope>ABUWG</scope><scope>AEUYN</scope><scope>AFKRA</scope><scope>ARAPS</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>BHPHI</scope><scope>BKSAR</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>GNUQQ</scope><scope>H8D</scope><scope>HCIFZ</scope><scope>KL.</scope><scope>L7M</scope><scope>M2P</scope><scope>P5Z</scope><scope>P62</scope><scope>PCBAR</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>Q9U</scope></search><sort><creationdate>201212</creationdate><title>Oxygen and hydrogen ion abundance in the near-Earth magnetosphere: Statistical results on the response to the geomagnetic and solar wind activity conditions</title><author>Kronberg, E. A. ; Haaland, S. E. ; Daly, P. W. ; Grigorenko, E. E. ; Kistler, L. M. ; Fränz, M. ; Dandouras, I.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c4493-21d5c1ec86955bc3379ce57163cba6953a48073551a47f22e869d5c90717ce683</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2012</creationdate><topic>Atmospheric sciences</topic><topic>Earth</topic><topic>Hydrogen ions</topic><topic>Magnetic fields</topic><topic>Magnetism</topic><topic>oxygen abundance</topic><topic>Plasma physics</topic><topic>response to solar wind</topic><topic>Space</topic><topic>storm</topic><topic>substorms</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Kronberg, E. A.</creatorcontrib><creatorcontrib>Haaland, S. E.</creatorcontrib><creatorcontrib>Daly, P. W.</creatorcontrib><creatorcontrib>Grigorenko, E. E.</creatorcontrib><creatorcontrib>Kistler, L. M.</creatorcontrib><creatorcontrib>Fränz, M.</creatorcontrib><creatorcontrib>Dandouras, I.</creatorcontrib><collection>Istex</collection><collection>CrossRef</collection><collection>ProQuest Central (Corporate)</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>ProQuest Central (purchase pre-March 2016)</collection><collection>Science Database (Alumni Edition)</collection><collection>Technology Research Database</collection><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>ProQuest Central (Alumni) (purchase pre-March 2016)</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest One Sustainability</collection><collection>ProQuest Central UK/Ireland</collection><collection>Advanced Technologies & Aerospace Collection</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>Natural Science Collection</collection><collection>Earth, Atmospheric & Aquatic Science Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>ProQuest Central Student</collection><collection>Aerospace Database</collection><collection>SciTech Premium Collection</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Science Database</collection><collection>Advanced Technologies & Aerospace Database</collection><collection>ProQuest Advanced Technologies & Aerospace Collection</collection><collection>Earth, Atmospheric & Aquatic Science Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central Basic</collection><jtitle>Journal of Geophysical Research: Space Physics</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Kronberg, E. A.</au><au>Haaland, S. E.</au><au>Daly, P. W.</au><au>Grigorenko, E. E.</au><au>Kistler, L. M.</au><au>Fränz, M.</au><au>Dandouras, I.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Oxygen and hydrogen ion abundance in the near-Earth magnetosphere: Statistical results on the response to the geomagnetic and solar wind activity conditions</atitle><jtitle>Journal of Geophysical Research: Space Physics</jtitle><addtitle>J. Geophys. Res</addtitle><date>2012-12</date><risdate>2012</risdate><volume>117</volume><issue>A12</issue><epage>n/a</epage><issn>0148-0227</issn><issn>2169-9380</issn><eissn>2156-2202</eissn><eissn>2169-9402</eissn><abstract>The composition of ions plays a crucial role for the fundamental plasma properties in the terrestrial magnetosphere. We investigate the oxygen‐to‐hydrogen ratio in the near‐Earth magnetosphere from −10 RE < XGSE < 10 RE. The results are based on seven years of ion flux measurements in the energy range ∼10 keV to ∼955 keV from the RAPID and CIS instruments on board the Cluster satellites. We find that (1) hydrogen ions at ∼10 keV show only a slight correlation with the geomagnetic conditions and interplanetary magnetic field changes. They are best correlated with the solar wind dynamic pressure and density, which is an expected effect of the magnetospheric compression; (2) ∼10 keV O+ ion intensities are more strongly affected during disturbed phase of a geomagnetic storm or substorm than >274 keV O+ ion intensities, relative to the corresponding hydrogen intensities; (3) In contrast to ∼10 keV ions, the >274 keV O+ions show the strongest acceleration during growth phase and not during the expansion phase itself. This suggests a connection between the energy input to the magnetosphere and the effective energization of energetic ions during growth phase; (4) The ratio between quiet and disturbed times for the intensities of ion ionospheric outflow is similar to those observed in the near‐Earth magnetosphere at >274 keV. Therefore, the increase of the energetic ion intensity during disturbed time is likely due to the intensification and the effective acceleration of the ionospheric source. In conclusion, the energization process in the near‐Earth magnetosphere is mass dependent and it is more effective for the heavier ions.
Key Points
Response of the O+ and H+ to the geomagnetic and solar wind changes
The strongest energetic O+ acceleration is during growth phase
O+ at lower energies is strongly affected by storms and substorms</abstract><cop>Washington</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1029/2012JA018071</doi><tpages>13</tpages><oa>free_for_read</oa></addata></record> |
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| source | Wiley Online Library Journals Frontfile Complete; Wiley Free Content; Wiley-Blackwell AGU Digital Library; Alma/SFX Local Collection |
| subjects | Atmospheric sciences Earth Hydrogen ions Magnetic fields Magnetism oxygen abundance Plasma physics response to solar wind Space storm substorms |
| title | Oxygen and hydrogen ion abundance in the near-Earth magnetosphere: Statistical results on the response to the geomagnetic and solar wind activity conditions |
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