Correlation analysis of field-aligned currents from the magnetic measurements of GRACE follow-on mission

Abstract In this study we performed a detailed analysis on the scale-size of field-aligned currents (FACs) at auroral latitudes, using the well-calibrated magnetic data from the non-dedicated magnetic field mission, Gravity Recovery and Climate Experiment Follow-On (GRACE-FO). With two spacecraft fo...

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Autores principales: Chao Xiong, Claudia Stolle, Ingo Michaelis, Hermann Lühr, Yunliang Zhou, Hui Wang, Guram Kervalishvili, Jan Rauberg
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spelling oai:doaj.org-article:b0b9768f05f74df5980cf737b7120cc22021-11-21T12:30:48ZCorrelation analysis of field-aligned currents from the magnetic measurements of GRACE follow-on mission10.1186/s40623-021-01540-y1880-5981https://doaj.org/article/b0b9768f05f74df5980cf737b7120cc22021-11-01T00:00:00Zhttps://doi.org/10.1186/s40623-021-01540-yhttps://doaj.org/toc/1880-5981Abstract In this study we performed a detailed analysis on the scale-size of field-aligned currents (FACs) at auroral latitudes, using the well-calibrated magnetic data from the non-dedicated magnetic field mission, Gravity Recovery and Climate Experiment Follow-On (GRACE-FO). With two spacecraft following each other, the GRACE-FO provides a good opportunity to identify the variation of FACs with different scale lengths. The results show that the auroral FACs can be classified into two groups: the small-scale ones, shorter than some tens of kilometers, dominated by kinetic Alfvén waves, are quite dynamic; and the large-scale ones, typically larger than 150 km, can be considered as quasi-static and persist longer than 1 min. The GRACE-FO observations also reveal that the small-scale FACs at the same location sometimes can persist over 25 s, e.g., around dusk and dawn hours, which is longer than the typical persistent period (10 s) of kinetic Alfvén waves as earlier reported. The FAC structures show clear magnetic local time dependence, with higher correlations between the spacecraft around dusk and dawn hours; lower correlations are found around midnight and lowest correlations around noon, implying that the small-scale FACs most frequently appear at the noon cusp region. Slightly better correlations of FACs between two spacecraft are found during local summer, and such seasonal dependence is dominated by the correlations of small-scale FACs at noon. However, further analysis shows that the small-scale FACs at noon have largest occurrence and intensity during local summer, which reveals that when interpreting the cross-correlation analysis the intensity of FACs needs to be taken into account. Graphical AbstractChao XiongClaudia StolleIngo MichaelisHermann LührYunliang ZhouHui WangGuram KervalishviliJan RaubergSpringerOpenarticleGeography. Anthropology. RecreationGGeodesyQB275-343GeologyQE1-996.5ENEarth, Planets and Space, Vol 73, Iss 1, Pp 1-13 (2021)
institution DOAJ
collection DOAJ
language EN
topic Geography. Anthropology. Recreation
G
Geodesy
QB275-343
Geology
QE1-996.5
spellingShingle Geography. Anthropology. Recreation
G
Geodesy
QB275-343
Geology
QE1-996.5
Chao Xiong
Claudia Stolle
Ingo Michaelis
Hermann Lühr
Yunliang Zhou
Hui Wang
Guram Kervalishvili
Jan Rauberg
Correlation analysis of field-aligned currents from the magnetic measurements of GRACE follow-on mission
description Abstract In this study we performed a detailed analysis on the scale-size of field-aligned currents (FACs) at auroral latitudes, using the well-calibrated magnetic data from the non-dedicated magnetic field mission, Gravity Recovery and Climate Experiment Follow-On (GRACE-FO). With two spacecraft following each other, the GRACE-FO provides a good opportunity to identify the variation of FACs with different scale lengths. The results show that the auroral FACs can be classified into two groups: the small-scale ones, shorter than some tens of kilometers, dominated by kinetic Alfvén waves, are quite dynamic; and the large-scale ones, typically larger than 150 km, can be considered as quasi-static and persist longer than 1 min. The GRACE-FO observations also reveal that the small-scale FACs at the same location sometimes can persist over 25 s, e.g., around dusk and dawn hours, which is longer than the typical persistent period (10 s) of kinetic Alfvén waves as earlier reported. The FAC structures show clear magnetic local time dependence, with higher correlations between the spacecraft around dusk and dawn hours; lower correlations are found around midnight and lowest correlations around noon, implying that the small-scale FACs most frequently appear at the noon cusp region. Slightly better correlations of FACs between two spacecraft are found during local summer, and such seasonal dependence is dominated by the correlations of small-scale FACs at noon. However, further analysis shows that the small-scale FACs at noon have largest occurrence and intensity during local summer, which reveals that when interpreting the cross-correlation analysis the intensity of FACs needs to be taken into account. Graphical Abstract
format article
author Chao Xiong
Claudia Stolle
Ingo Michaelis
Hermann Lühr
Yunliang Zhou
Hui Wang
Guram Kervalishvili
Jan Rauberg
author_facet Chao Xiong
Claudia Stolle
Ingo Michaelis
Hermann Lühr
Yunliang Zhou
Hui Wang
Guram Kervalishvili
Jan Rauberg
author_sort Chao Xiong
title Correlation analysis of field-aligned currents from the magnetic measurements of GRACE follow-on mission
title_short Correlation analysis of field-aligned currents from the magnetic measurements of GRACE follow-on mission
title_full Correlation analysis of field-aligned currents from the magnetic measurements of GRACE follow-on mission
title_fullStr Correlation analysis of field-aligned currents from the magnetic measurements of GRACE follow-on mission
title_full_unstemmed Correlation analysis of field-aligned currents from the magnetic measurements of GRACE follow-on mission
title_sort correlation analysis of field-aligned currents from the magnetic measurements of grace follow-on mission
publisher SpringerOpen
publishDate 2021
url https://doaj.org/article/b0b9768f05f74df5980cf737b7120cc2
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