ULF geomagnetic pulsations at different latitudes in Antarctica
We present a study aimed to characterize the ULF (1–100 mHz) geomagnetic pulsation activity in the polar cap at different latitudes. We used magnetic measurements obtained through 2005–2007 in Antarctica, at Dome C (89° S corrected geomagnetic latitude) and at Terra Nova Bay (80° S corrected geomagn...
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ftdoajarticles:oai:doaj.org/article:a48d5f5063f644feb78caa17c248e90b 2023-05-15T13:49:32+02:00 ULF geomagnetic pulsations at different latitudes in Antarctica P. Francia M. De Lauretis M. Vellante U. Villante A. Piancatelli 2009-09-01T00:00:00Z https://doi.org/10.5194/angeo-27-3621-2009 https://doaj.org/article/a48d5f5063f644feb78caa17c248e90b EN eng Copernicus Publications https://www.ann-geophys.net/27/3621/2009/angeo-27-3621-2009.pdf https://doaj.org/toc/0992-7689 https://doaj.org/toc/1432-0576 doi:10.5194/angeo-27-3621-2009 0992-7689 1432-0576 https://doaj.org/article/a48d5f5063f644feb78caa17c248e90b Annales Geophysicae, Vol 27, Pp 3621-3629 (2009) Science Q Physics QC1-999 Geophysics. Cosmic physics QC801-809 article 2009 ftdoajarticles https://doi.org/10.5194/angeo-27-3621-2009 2022-12-31T14:54:54Z We present a study aimed to characterize the ULF (1–100 mHz) geomagnetic pulsation activity in the polar cap at different latitudes. We used magnetic measurements obtained through 2005–2007 in Antarctica, at Dome C (89° S corrected geomagnetic latitude) and at Terra Nova Bay (80° S corrected geomagnetic latitude). The results indicate a solar wind control of the wave activity, more important at larger distances from the cusp, as well as a significant role of the local ionospheric conditions. The different position of the two stations, with respect to the cusp and closed field lines, is responsible for the observed different pulsation characteristics. At Terra Nova Bay, due to the approaching of the station to the cusp and closed field lines in the daytime, the ULF power is characterized by a maximum around noon; daytime pulsation events in the Pc5 frequency band are related to the fundamental field line resonances occurring at lower latitudes, while higher harmonics of the fundamental may account for the characteristics of Pc3–4 pulsations. In the nighttime, at Pc3 frequencies, the results suggest waves propagating sunward, possibly due to the transmission of upstream waves from the magnetosheath via the magnetotail lobes. At Dome C, near the geomagnetic pole and very far from closed field lines, the ULF power in any frequency band only shows an enhancement in the postmidnight sector, more pronounced for Pc3 pulsations. The ULF activity appears to be driven by processes occurring in the magnetotail: in particular, nighttime Pc3 pulsation events may be originated from upstream wave penetration through the magnetotail lobes. Article in Journal/Newspaper Antarc* Antarctica Geomagnetic Pole Directory of Open Access Journals: DOAJ Articles Terra Nova Bay Annales Geophysicae 27 9 3621 3629 |
institution |
Open Polar |
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Directory of Open Access Journals: DOAJ Articles |
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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 P. Francia M. De Lauretis M. Vellante U. Villante A. Piancatelli ULF geomagnetic pulsations at different latitudes in Antarctica |
topic_facet |
Science Q Physics QC1-999 Geophysics. Cosmic physics QC801-809 |
description |
We present a study aimed to characterize the ULF (1–100 mHz) geomagnetic pulsation activity in the polar cap at different latitudes. We used magnetic measurements obtained through 2005–2007 in Antarctica, at Dome C (89° S corrected geomagnetic latitude) and at Terra Nova Bay (80° S corrected geomagnetic latitude). The results indicate a solar wind control of the wave activity, more important at larger distances from the cusp, as well as a significant role of the local ionospheric conditions. The different position of the two stations, with respect to the cusp and closed field lines, is responsible for the observed different pulsation characteristics. At Terra Nova Bay, due to the approaching of the station to the cusp and closed field lines in the daytime, the ULF power is characterized by a maximum around noon; daytime pulsation events in the Pc5 frequency band are related to the fundamental field line resonances occurring at lower latitudes, while higher harmonics of the fundamental may account for the characteristics of Pc3–4 pulsations. In the nighttime, at Pc3 frequencies, the results suggest waves propagating sunward, possibly due to the transmission of upstream waves from the magnetosheath via the magnetotail lobes. At Dome C, near the geomagnetic pole and very far from closed field lines, the ULF power in any frequency band only shows an enhancement in the postmidnight sector, more pronounced for Pc3 pulsations. The ULF activity appears to be driven by processes occurring in the magnetotail: in particular, nighttime Pc3 pulsation events may be originated from upstream wave penetration through the magnetotail lobes. |
format |
Article in Journal/Newspaper |
author |
P. Francia M. De Lauretis M. Vellante U. Villante A. Piancatelli |
author_facet |
P. Francia M. De Lauretis M. Vellante U. Villante A. Piancatelli |
author_sort |
P. Francia |
title |
ULF geomagnetic pulsations at different latitudes in Antarctica |
title_short |
ULF geomagnetic pulsations at different latitudes in Antarctica |
title_full |
ULF geomagnetic pulsations at different latitudes in Antarctica |
title_fullStr |
ULF geomagnetic pulsations at different latitudes in Antarctica |
title_full_unstemmed |
ULF geomagnetic pulsations at different latitudes in Antarctica |
title_sort |
ulf geomagnetic pulsations at different latitudes in antarctica |
publisher |
Copernicus Publications |
publishDate |
2009 |
url |
https://doi.org/10.5194/angeo-27-3621-2009 https://doaj.org/article/a48d5f5063f644feb78caa17c248e90b |
geographic |
Terra Nova Bay |
geographic_facet |
Terra Nova Bay |
genre |
Antarc* Antarctica Geomagnetic Pole |
genre_facet |
Antarc* Antarctica Geomagnetic Pole |
op_source |
Annales Geophysicae, Vol 27, Pp 3621-3629 (2009) |
op_relation |
https://www.ann-geophys.net/27/3621/2009/angeo-27-3621-2009.pdf https://doaj.org/toc/0992-7689 https://doaj.org/toc/1432-0576 doi:10.5194/angeo-27-3621-2009 0992-7689 1432-0576 https://doaj.org/article/a48d5f5063f644feb78caa17c248e90b |
op_doi |
https://doi.org/10.5194/angeo-27-3621-2009 |
container_title |
Annales Geophysicae |
container_volume |
27 |
container_issue |
9 |
container_start_page |
3621 |
op_container_end_page |
3629 |
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1766251474615009280 |