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Statistical characteristics of the storm time plasma sheet
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| Zeitschriftentitel: | Journal of Geophysical Research: Space Physics |
|---|---|
| Personen und Körperschaften: | , |
| In: | Journal of Geophysical Research: Space Physics, 113, 2008, A1 |
| Format: | E-Article |
| Sprache: | Englisch |
| veröffentlicht: |
American Geophysical Union (AGU)
|
| Schlagwörter: |
| author_facet |
Ohtani, S. Mukai, T. Ohtani, S. Mukai, T. |
|---|---|
| author |
Ohtani, S. Mukai, T. |
| spellingShingle |
Ohtani, S. Mukai, T. Journal of Geophysical Research: Space Physics Statistical characteristics of the storm time plasma sheet Paleontology Space and Planetary Science Earth and Planetary Sciences (miscellaneous) Atmospheric Science Earth-Surface Processes Geochemistry and Petrology Soil Science Water Science and Technology Ecology Aquatic Science Forestry Oceanography Geophysics |
| author_sort |
ohtani, s. |
| spelling |
Ohtani, S. Mukai, T. 0148-0227 American Geophysical Union (AGU) Paleontology Space and Planetary Science Earth and Planetary Sciences (miscellaneous) Atmospheric Science Earth-Surface Processes Geochemistry and Petrology Soil Science Water Science and Technology Ecology Aquatic Science Forestry Oceanography Geophysics http://dx.doi.org/10.1029/2007ja012547 <jats:p>The present study addresses the convection and configuration of the storm time plasma sheet by examining the occurrence ratios of fundamental plasma quantities. Measurements made by the Geotail spacecraft in the midnight sector are used. The results are summarized as follows: (1) the occurrence ratio of the plasma flow velocity is not noticeably different between storm and nonstorm time or between the main and recovery phases; (2) the convection electric field is more intense during the main phase; (3) the equatorial magnetic field is stronger during the main phase; (4) the ion pressure is higher, therefore the tail current is more intense, during the main phase. It is suggested that the stronger equatorial magnetic field (result 3) counteracts the enhancement of the convection electric field (result 2) so that the occurrence ratio of the flow velocity does not depends on geomagnetic activity (result 1). The storm time increase in the equatorial magnetic field can be attributed to the <jats:italic>X</jats:italic>‐dependent intensification of the dawn‐to‐dusk electric current (the ring current and tail current); if the current is more intensified on the earthward side than on the tailward side, the net change in <jats:italic>B</jats:italic><jats:sub><jats:italic>Z</jats:italic></jats:sub> is positive. It is also found that the reconnection takes place, if infrequently, at <jats:italic>X</jats:italic> > −15 <jats:italic>R</jats:italic><jats:sub><jats:italic>E</jats:italic></jats:sub> during storm periods. However, result 1 suggests that despite the intense tail current (result 4), the <jats:italic>X</jats:italic> distribution of the near‐Earth reconnection site does not statistically depend on storm activity. This can also be attributed to the stronger equatorial magnetic field as well as to the storm time enhancement of the near‐Earth plasma number density. It is therefore suggested that the ring current affects the plasma sheet dynamics through its contribution to the tail magnetic configuration.</jats:p> Statistical characteristics of the storm time plasma sheet Journal of Geophysical Research: Space Physics |
| doi_str_mv |
10.1029/2007ja012547 |
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Online Free |
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Technik Geologie und Paläontologie Geographie Chemie und Pharmazie Land- und Forstwirtschaft, Gartenbau, Fischereiwirtschaft, Hauswirtschaft Biologie Allgemeine Naturwissenschaft Physik |
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American Geophysical Union (AGU), 2008 |
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American Geophysical Union (AGU), 2008 |
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Journal of Geophysical Research: Space Physics |
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| title |
Statistical characteristics of the storm time plasma sheet |
| title_unstemmed |
Statistical characteristics of the storm time plasma sheet |
| title_full |
Statistical characteristics of the storm time plasma sheet |
| title_fullStr |
Statistical characteristics of the storm time plasma sheet |
| title_full_unstemmed |
Statistical characteristics of the storm time plasma sheet |
| title_short |
Statistical characteristics of the storm time plasma sheet |
| title_sort |
statistical characteristics of the storm time plasma sheet |
| topic |
Paleontology Space and Planetary Science Earth and Planetary Sciences (miscellaneous) Atmospheric Science Earth-Surface Processes Geochemistry and Petrology Soil Science Water Science and Technology Ecology Aquatic Science Forestry Oceanography Geophysics |
| url |
http://dx.doi.org/10.1029/2007ja012547 |
| publishDate |
2008 |
| physical |
|
| description |
<jats:p>The present study addresses the convection and configuration of the storm time plasma sheet by examining the occurrence ratios of fundamental plasma quantities. Measurements made by the Geotail spacecraft in the midnight sector are used. The results are summarized as follows: (1) the occurrence ratio of the plasma flow velocity is not noticeably different between storm and nonstorm time or between the main and recovery phases; (2) the convection electric field is more intense during the main phase; (3) the equatorial magnetic field is stronger during the main phase; (4) the ion pressure is higher, therefore the tail current is more intense, during the main phase. It is suggested that the stronger equatorial magnetic field (result 3) counteracts the enhancement of the convection electric field (result 2) so that the occurrence ratio of the flow velocity does not depends on geomagnetic activity (result 1). The storm time increase in the equatorial magnetic field can be attributed to the <jats:italic>X</jats:italic>‐dependent intensification of the dawn‐to‐dusk electric current (the ring current and tail current); if the current is more intensified on the earthward side than on the tailward side, the net change in <jats:italic>B</jats:italic><jats:sub><jats:italic>Z</jats:italic></jats:sub> is positive. It is also found that the reconnection takes place, if infrequently, at <jats:italic>X</jats:italic> > −15 <jats:italic>R</jats:italic><jats:sub><jats:italic>E</jats:italic></jats:sub> during storm periods. However, result 1 suggests that despite the intense tail current (result 4), the <jats:italic>X</jats:italic> distribution of the near‐Earth reconnection site does not statistically depend on storm activity. This can also be attributed to the stronger equatorial magnetic field as well as to the storm time enhancement of the near‐Earth plasma number density. It is therefore suggested that the ring current affects the plasma sheet dynamics through its contribution to the tail magnetic configuration.</jats:p> |
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| author | Ohtani, S., Mukai, T. |
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| author_sort | ohtani, s. |
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| container_title | Journal of Geophysical Research: Space Physics |
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| description | <jats:p>The present study addresses the convection and configuration of the storm time plasma sheet by examining the occurrence ratios of fundamental plasma quantities. Measurements made by the Geotail spacecraft in the midnight sector are used. The results are summarized as follows: (1) the occurrence ratio of the plasma flow velocity is not noticeably different between storm and nonstorm time or between the main and recovery phases; (2) the convection electric field is more intense during the main phase; (3) the equatorial magnetic field is stronger during the main phase; (4) the ion pressure is higher, therefore the tail current is more intense, during the main phase. It is suggested that the stronger equatorial magnetic field (result 3) counteracts the enhancement of the convection electric field (result 2) so that the occurrence ratio of the flow velocity does not depends on geomagnetic activity (result 1). The storm time increase in the equatorial magnetic field can be attributed to the <jats:italic>X</jats:italic>‐dependent intensification of the dawn‐to‐dusk electric current (the ring current and tail current); if the current is more intensified on the earthward side than on the tailward side, the net change in <jats:italic>B</jats:italic><jats:sub><jats:italic>Z</jats:italic></jats:sub> is positive. It is also found that the reconnection takes place, if infrequently, at <jats:italic>X</jats:italic> > −15 <jats:italic>R</jats:italic><jats:sub><jats:italic>E</jats:italic></jats:sub> during storm periods. However, result 1 suggests that despite the intense tail current (result 4), the <jats:italic>X</jats:italic> distribution of the near‐Earth reconnection site does not statistically depend on storm activity. This can also be attributed to the stronger equatorial magnetic field as well as to the storm time enhancement of the near‐Earth plasma number density. It is therefore suggested that the ring current affects the plasma sheet dynamics through its contribution to the tail magnetic configuration.</jats:p> |
| doi_str_mv | 10.1029/2007ja012547 |
| facet_avail | Online, Free |
| finc_class_facet | Technik, Geologie und Paläontologie, Geographie, Chemie und Pharmazie, Land- und Forstwirtschaft, Gartenbau, Fischereiwirtschaft, Hauswirtschaft, Biologie, Allgemeine Naturwissenschaft, Physik |
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| format_de14 | Article, E-Article |
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| id | ai-49-aHR0cDovL2R4LmRvaS5vcmcvMTAuMTAyOS8yMDA3amEwMTI1NDc |
| imprint | American Geophysical Union (AGU), 2008 |
| imprint_str_mv | American Geophysical Union (AGU), 2008 |
| institution | DE-D275, DE-Bn3, DE-Brt1, DE-Zwi2, DE-D161, DE-Gla1, DE-Zi4, DE-15, DE-Pl11, DE-Rs1, DE-105, DE-14, DE-Ch1, DE-L229 |
| issn | 0148-0227 |
| issn_str_mv | 0148-0227 |
| language | English |
| last_indexed | 2024-03-01T15:33:59.187Z |
| match_str | ohtani2008statisticalcharacteristicsofthestormtimeplasmasheet |
| mega_collection | American Geophysical Union (AGU) (CrossRef) |
| physical | |
| publishDate | 2008 |
| publishDateSort | 2008 |
| publisher | American Geophysical Union (AGU) |
| record_format | ai |
| recordtype | ai |
| series | Journal of Geophysical Research: Space Physics |
| source_id | 49 |
| spelling | Ohtani, S. Mukai, T. 0148-0227 American Geophysical Union (AGU) Paleontology Space and Planetary Science Earth and Planetary Sciences (miscellaneous) Atmospheric Science Earth-Surface Processes Geochemistry and Petrology Soil Science Water Science and Technology Ecology Aquatic Science Forestry Oceanography Geophysics http://dx.doi.org/10.1029/2007ja012547 <jats:p>The present study addresses the convection and configuration of the storm time plasma sheet by examining the occurrence ratios of fundamental plasma quantities. Measurements made by the Geotail spacecraft in the midnight sector are used. The results are summarized as follows: (1) the occurrence ratio of the plasma flow velocity is not noticeably different between storm and nonstorm time or between the main and recovery phases; (2) the convection electric field is more intense during the main phase; (3) the equatorial magnetic field is stronger during the main phase; (4) the ion pressure is higher, therefore the tail current is more intense, during the main phase. It is suggested that the stronger equatorial magnetic field (result 3) counteracts the enhancement of the convection electric field (result 2) so that the occurrence ratio of the flow velocity does not depends on geomagnetic activity (result 1). The storm time increase in the equatorial magnetic field can be attributed to the <jats:italic>X</jats:italic>‐dependent intensification of the dawn‐to‐dusk electric current (the ring current and tail current); if the current is more intensified on the earthward side than on the tailward side, the net change in <jats:italic>B</jats:italic><jats:sub><jats:italic>Z</jats:italic></jats:sub> is positive. It is also found that the reconnection takes place, if infrequently, at <jats:italic>X</jats:italic> > −15 <jats:italic>R</jats:italic><jats:sub><jats:italic>E</jats:italic></jats:sub> during storm periods. However, result 1 suggests that despite the intense tail current (result 4), the <jats:italic>X</jats:italic> distribution of the near‐Earth reconnection site does not statistically depend on storm activity. This can also be attributed to the stronger equatorial magnetic field as well as to the storm time enhancement of the near‐Earth plasma number density. It is therefore suggested that the ring current affects the plasma sheet dynamics through its contribution to the tail magnetic configuration.</jats:p> Statistical characteristics of the storm time plasma sheet Journal of Geophysical Research: Space Physics |
| spellingShingle | Ohtani, S., Mukai, T., Journal of Geophysical Research: Space Physics, Statistical characteristics of the storm time plasma sheet, Paleontology, Space and Planetary Science, Earth and Planetary Sciences (miscellaneous), Atmospheric Science, Earth-Surface Processes, Geochemistry and Petrology, Soil Science, Water Science and Technology, Ecology, Aquatic Science, Forestry, Oceanography, Geophysics |
| title | Statistical characteristics of the storm time plasma sheet |
| title_full | Statistical characteristics of the storm time plasma sheet |
| title_fullStr | Statistical characteristics of the storm time plasma sheet |
| title_full_unstemmed | Statistical characteristics of the storm time plasma sheet |
| title_short | Statistical characteristics of the storm time plasma sheet |
| title_sort | statistical characteristics of the storm time plasma sheet |
| title_unstemmed | Statistical characteristics of the storm time plasma sheet |
| topic | Paleontology, Space and Planetary Science, Earth and Planetary Sciences (miscellaneous), Atmospheric Science, Earth-Surface Processes, Geochemistry and Petrology, Soil Science, Water Science and Technology, Ecology, Aquatic Science, Forestry, Oceanography, Geophysics |
| url | http://dx.doi.org/10.1029/2007ja012547 |