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The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion
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| Zeitschriftentitel: | Annales Geophysicae |
|---|---|
| Personen und Körperschaften: | , |
| In: | Annales Geophysicae, 33, 2015, 1, S. 39-46 |
| Format: | E-Article |
| Sprache: | Englisch |
| veröffentlicht: |
Copernicus GmbH
|
| Schlagwörter: |
| author_facet |
Wing, S. Zhang, Y. L. Wing, S. Zhang, Y. L. |
|---|---|
| author |
Wing, S. Zhang, Y. L. |
| spellingShingle |
Wing, S. Zhang, Y. L. Annales Geophysicae The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion Space and Planetary Science Earth and Planetary Sciences (miscellaneous) Atmospheric Science Geology Astronomy and Astrophysics |
| author_sort |
wing, s. |
| spelling |
Wing, S. Zhang, Y. L. 1432-0576 Copernicus GmbH Space and Planetary Science Earth and Planetary Sciences (miscellaneous) Atmospheric Science Geology Astronomy and Astrophysics http://dx.doi.org/10.5194/angeo-33-39-2015 <jats:p>Abstract. The polar rain electrons near the open–closed field line boundary on the nightside often exhibit energy-latitude dispersion, in which the energy decreases with decreasing latitude. The solar wind electrons from the last open-field line would E × B drift equatorward as they move toward the ionosphere, resulting in the observed dispersion. This process is modeled successfully by an open-field line particle precipitation model. The existing method for determining the magnetotail X line distance from the electron dispersion underestimates the electron path length from the X line to the ionosphere by at least 33%. The best estimate of the path length comes from using the two highest energy electrons in the dispersion region. The magnetic field line open–closed boundary is located poleward of the highest energy electrons in the dispersion region, which in turn is located poleward of Defense Meteorological Satellite Program (DMSP) b6, b5e, and b5i boundaries. In the four events examined, b6 is located at least 0.7–1.5° equatorward of the magnetic field line open–closed boundary. The energy-latitude dispersion seen in the electron overhang may result from the plasma sheet electron curvature and gradient drifts into the newly closed field line. </jats:p> The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion Annales Geophysicae |
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The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| title_unstemmed |
The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| title_full |
The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| title_fullStr |
The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| title_full_unstemmed |
The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| title_short |
The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| title_sort |
the nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| topic |
Space and Planetary Science Earth and Planetary Sciences (miscellaneous) Atmospheric Science Geology Astronomy and Astrophysics |
| url |
http://dx.doi.org/10.5194/angeo-33-39-2015 |
| publishDate |
2015 |
| physical |
39-46 |
| description |
<jats:p>Abstract. The polar rain electrons near the open–closed field line boundary on the nightside often exhibit energy-latitude dispersion, in which the energy decreases with decreasing latitude. The solar wind electrons from the last open-field line would E × B drift equatorward as they move toward the ionosphere, resulting in the observed dispersion. This process is modeled successfully by an open-field line particle precipitation model. The existing method for determining the magnetotail X line distance from the electron dispersion underestimates the electron path length from the X line to the ionosphere by at least 33%. The best estimate of the path length comes from using the two highest energy electrons in the dispersion region. The magnetic field line open–closed boundary is located poleward of the highest energy electrons in the dispersion region, which in turn is located poleward of Defense Meteorological Satellite Program (DMSP) b6, b5e, and b5i boundaries. In the four events examined, b6 is located at least 0.7–1.5° equatorward of the magnetic field line open–closed boundary. The energy-latitude dispersion seen in the electron overhang may result from the plasma sheet electron curvature and gradient drifts into the newly closed field line.
</jats:p> |
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| description | <jats:p>Abstract. The polar rain electrons near the open–closed field line boundary on the nightside often exhibit energy-latitude dispersion, in which the energy decreases with decreasing latitude. The solar wind electrons from the last open-field line would E × B drift equatorward as they move toward the ionosphere, resulting in the observed dispersion. This process is modeled successfully by an open-field line particle precipitation model. The existing method for determining the magnetotail X line distance from the electron dispersion underestimates the electron path length from the X line to the ionosphere by at least 33%. The best estimate of the path length comes from using the two highest energy electrons in the dispersion region. The magnetic field line open–closed boundary is located poleward of the highest energy electrons in the dispersion region, which in turn is located poleward of Defense Meteorological Satellite Program (DMSP) b6, b5e, and b5i boundaries. In the four events examined, b6 is located at least 0.7–1.5° equatorward of the magnetic field line open–closed boundary. The energy-latitude dispersion seen in the electron overhang may result from the plasma sheet electron curvature and gradient drifts into the newly closed field line. </jats:p> |
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| spelling | Wing, S. Zhang, Y. L. 1432-0576 Copernicus GmbH Space and Planetary Science Earth and Planetary Sciences (miscellaneous) Atmospheric Science Geology Astronomy and Astrophysics http://dx.doi.org/10.5194/angeo-33-39-2015 <jats:p>Abstract. The polar rain electrons near the open–closed field line boundary on the nightside often exhibit energy-latitude dispersion, in which the energy decreases with decreasing latitude. The solar wind electrons from the last open-field line would E × B drift equatorward as they move toward the ionosphere, resulting in the observed dispersion. This process is modeled successfully by an open-field line particle precipitation model. The existing method for determining the magnetotail X line distance from the electron dispersion underestimates the electron path length from the X line to the ionosphere by at least 33%. The best estimate of the path length comes from using the two highest energy electrons in the dispersion region. The magnetic field line open–closed boundary is located poleward of the highest energy electrons in the dispersion region, which in turn is located poleward of Defense Meteorological Satellite Program (DMSP) b6, b5e, and b5i boundaries. In the four events examined, b6 is located at least 0.7–1.5° equatorward of the magnetic field line open–closed boundary. The energy-latitude dispersion seen in the electron overhang may result from the plasma sheet electron curvature and gradient drifts into the newly closed field line. </jats:p> The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion Annales Geophysicae |
| spellingShingle | Wing, S., Zhang, Y. L., Annales Geophysicae, The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion, Space and Planetary Science, Earth and Planetary Sciences (miscellaneous), Atmospheric Science, Geology, Astronomy and Astrophysics |
| title | The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| title_full | The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| title_fullStr | The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| title_full_unstemmed | The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| title_short | The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| title_sort | the nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| title_unstemmed | The nightside magnetic field line open–closed boundary and polar rain electron energy-latitude dispersion |
| topic | Space and Planetary Science, Earth and Planetary Sciences (miscellaneous), Atmospheric Science, Geology, Astronomy and Astrophysics |
| url | http://dx.doi.org/10.5194/angeo-33-39-2015 |