IMF B y effects in the plasma flow at the polar cap boundary
We used the dataset obtained from the EISCAT Svalbard Radar during 2000–2008 to study statistically the ionospheric convection in a vicinity of the polar cap boundary as related to IMF B y conditions separately for northward and southward IMF. The effect of IMF B y is manifested in the intensity and...
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ftdoajarticles:oai:doaj.org/article:a4d778af4c6a4ffbaafb99d7f3107850 2023-05-15T16:04:46+02:00 IMF B y effects in the plasma flow at the polar cap boundary R. Lukianova A. Kozlovsky 2011-07-01T00:00:00Z https://doi.org/10.5194/angeo-29-1305-2011 https://doaj.org/article/a4d778af4c6a4ffbaafb99d7f3107850 EN eng Copernicus Publications https://www.ann-geophys.net/29/1305/2011/angeo-29-1305-2011.pdf https://doaj.org/toc/0992-7689 https://doaj.org/toc/1432-0576 doi:10.5194/angeo-29-1305-2011 0992-7689 1432-0576 https://doaj.org/article/a4d778af4c6a4ffbaafb99d7f3107850 Annales Geophysicae, Vol 29, Pp 1305-1315 (2011) Science Q Physics QC1-999 Geophysics. Cosmic physics QC801-809 article 2011 ftdoajarticles https://doi.org/10.5194/angeo-29-1305-2011 2022-12-31T10:52:33Z We used the dataset obtained from the EISCAT Svalbard Radar during 2000–2008 to study statistically the ionospheric convection in a vicinity of the polar cap boundary as related to IMF B y conditions separately for northward and southward IMF. The effect of IMF B y is manifested in the intensity and direction of the azimuthal component of ionospheric flow. The most significant effect is observed on the day and night sides whereas on dawn and dusk the effect is essentially less prominent. However, there is an asymmetry with respect to the noon-midnight meridian. On the day side the intensity of B y -related azimuthal flow is maximal exactly at noon, whereas on the night side the maximum is shifted toward the post-midnight hours (~03:00 MLT). On the dusk side the relative reduction of the azimuthal flow is much larger than that on the dawn side. Overall, the magnetospheric response to IMF B y seems to be stronger in the 00:00–12:00 MLT sector compared to the 12:00–24:00 MLTs. Quantitative characteristics of the IMF B y effect are presented and partly explained by the magnetospheric electric fields generated due to the solar wind and also by the position of open-closed boundary for different IMF orientation. Article in Journal/Newspaper EISCAT Svalbard Directory of Open Access Journals: DOAJ Articles Svalbard Annales Geophysicae 29 7 1305 1315 |
institution |
Open Polar |
collection |
Directory of Open Access Journals: DOAJ Articles |
op_collection_id |
ftdoajarticles |
language |
English |
topic |
Science Q Physics QC1-999 Geophysics. Cosmic physics QC801-809 |
spellingShingle |
Science Q Physics QC1-999 Geophysics. Cosmic physics QC801-809 R. Lukianova A. Kozlovsky IMF B y effects in the plasma flow at the polar cap boundary |
topic_facet |
Science Q Physics QC1-999 Geophysics. Cosmic physics QC801-809 |
description |
We used the dataset obtained from the EISCAT Svalbard Radar during 2000–2008 to study statistically the ionospheric convection in a vicinity of the polar cap boundary as related to IMF B y conditions separately for northward and southward IMF. The effect of IMF B y is manifested in the intensity and direction of the azimuthal component of ionospheric flow. The most significant effect is observed on the day and night sides whereas on dawn and dusk the effect is essentially less prominent. However, there is an asymmetry with respect to the noon-midnight meridian. On the day side the intensity of B y -related azimuthal flow is maximal exactly at noon, whereas on the night side the maximum is shifted toward the post-midnight hours (~03:00 MLT). On the dusk side the relative reduction of the azimuthal flow is much larger than that on the dawn side. Overall, the magnetospheric response to IMF B y seems to be stronger in the 00:00–12:00 MLT sector compared to the 12:00–24:00 MLTs. Quantitative characteristics of the IMF B y effect are presented and partly explained by the magnetospheric electric fields generated due to the solar wind and also by the position of open-closed boundary for different IMF orientation. |
format |
Article in Journal/Newspaper |
author |
R. Lukianova A. Kozlovsky |
author_facet |
R. Lukianova A. Kozlovsky |
author_sort |
R. Lukianova |
title |
IMF B y effects in the plasma flow at the polar cap boundary |
title_short |
IMF B y effects in the plasma flow at the polar cap boundary |
title_full |
IMF B y effects in the plasma flow at the polar cap boundary |
title_fullStr |
IMF B y effects in the plasma flow at the polar cap boundary |
title_full_unstemmed |
IMF B y effects in the plasma flow at the polar cap boundary |
title_sort |
imf b y effects in the plasma flow at the polar cap boundary |
publisher |
Copernicus Publications |
publishDate |
2011 |
url |
https://doi.org/10.5194/angeo-29-1305-2011 https://doaj.org/article/a4d778af4c6a4ffbaafb99d7f3107850 |
geographic |
Svalbard |
geographic_facet |
Svalbard |
genre |
EISCAT Svalbard |
genre_facet |
EISCAT Svalbard |
op_source |
Annales Geophysicae, Vol 29, Pp 1305-1315 (2011) |
op_relation |
https://www.ann-geophys.net/29/1305/2011/angeo-29-1305-2011.pdf https://doaj.org/toc/0992-7689 https://doaj.org/toc/1432-0576 doi:10.5194/angeo-29-1305-2011 0992-7689 1432-0576 https://doaj.org/article/a4d778af4c6a4ffbaafb99d7f3107850 |
op_doi |
https://doi.org/10.5194/angeo-29-1305-2011 |
container_title |
Annales Geophysicae |
container_volume |
29 |
container_issue |
7 |
container_start_page |
1305 |
op_container_end_page |
1315 |
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1766400394268770304 |