Study of the solar wind coupling to the time difference horizontal geomagnetic field
(2005) In Annales Geophysicae 23(5). p.19491957 Abstract
 The local ground geomagnetic field fluctuations (AB) are dominated by high frequencies and 83% of the power is located at periods of 32 min or less. By forming 10min rootmeansquare (RMS) of A B a major part of this variation is captured. Using measured geomagnetic induced currents (GIC), from a power grid transformer in Southern Sweden, it is shown that the 10min standard deviation GIC may be computed from a linear model using the RMS AX and Delta Y at Brorfelde (BFE: 11.67 degrees E, 55.63 degrees N), Denmark, and Uppsala (UPS: 17.35 degrees E, 59.90 degrees N), Sweden, with a correlation of 0.926 +/ 0.015. From recurrent neural network models, that are driven by solar wind data, it is shown that the log RMS Delta X and Delta Y at... (More)
 The local ground geomagnetic field fluctuations (AB) are dominated by high frequencies and 83% of the power is located at periods of 32 min or less. By forming 10min rootmeansquare (RMS) of A B a major part of this variation is captured. Using measured geomagnetic induced currents (GIC), from a power grid transformer in Southern Sweden, it is shown that the 10min standard deviation GIC may be computed from a linear model using the RMS AX and Delta Y at Brorfelde (BFE: 11.67 degrees E, 55.63 degrees N), Denmark, and Uppsala (UPS: 17.35 degrees E, 59.90 degrees N), Sweden, with a correlation of 0.926 +/ 0.015. From recurrent neural network models, that are driven by solar wind data, it is shown that the log RMS Delta X and Delta Y at the two locations may be predicted up to 30 min in advance with a correlation close to 0.8: 0.78 +/ 0.02 for both directions at BFE; 0.81 +/ 0.02 and 0.80 +/ 0.02 in the X and Ydirections, respectively, at UPS. The most important inputs to the models are the 10min averages of the solar wind magnetic field component B, and velocity V, and the 10min standard deviation of the proton number density a,. The average proton number density n has no influence. (Less)
Please use this url to cite or link to this publication:
http://lup.lub.lu.se/record/225108
 author
 Wintoft, Peter ^{LU}
 organization
 publishing date
 2005
 type
 Contribution to journal
 publication status
 published
 subject
 keywords
 rapid time variations, geomagnetism and paleomagnetism, magnetosphere interactions, Magnetospheric physics, Solar wind
 in
 Annales Geophysicae
 volume
 23
 issue
 5
 pages
 1949  1957
 publisher
 European Geosciences Union
 external identifiers

 wos:000231706400039
 scopus:24044442259
 ISSN
 14320576
 language
 English
 LU publication?
 yes
 id
 a4d3cbfae5874a2797790b79ff633c25 (old id 225108)
 alternative location
 http://www.anngeophys.net/23/1949/2005/angeo2319492005.pdf
 date added to LUP
 20071005 16:30:57
 date last changed
 20180107 06:22:39
@article{a4d3cbfae5874a2797790b79ff633c25, abstract = {The local ground geomagnetic field fluctuations (AB) are dominated by high frequencies and 83% of the power is located at periods of 32 min or less. By forming 10min rootmeansquare (RMS) of A B a major part of this variation is captured. Using measured geomagnetic induced currents (GIC), from a power grid transformer in Southern Sweden, it is shown that the 10min standard deviation GIC may be computed from a linear model using the RMS AX and Delta Y at Brorfelde (BFE: 11.67 degrees E, 55.63 degrees N), Denmark, and Uppsala (UPS: 17.35 degrees E, 59.90 degrees N), Sweden, with a correlation of 0.926 +/ 0.015. From recurrent neural network models, that are driven by solar wind data, it is shown that the log RMS Delta X and Delta Y at the two locations may be predicted up to 30 min in advance with a correlation close to 0.8: 0.78 +/ 0.02 for both directions at BFE; 0.81 +/ 0.02 and 0.80 +/ 0.02 in the X and Ydirections, respectively, at UPS. The most important inputs to the models are the 10min averages of the solar wind magnetic field component B, and velocity V, and the 10min standard deviation of the proton number density a,. The average proton number density n has no influence.}, author = {Wintoft, Peter}, issn = {14320576}, keyword = {rapid time variations,geomagnetism and paleomagnetism,magnetosphere interactions,Magnetospheric physics,Solar wind}, language = {eng}, number = {5}, pages = {19491957}, publisher = {European Geosciences Union}, series = {Annales Geophysicae}, title = {Study of the solar wind coupling to the time difference horizontal geomagnetic field}, volume = {23}, year = {2005}, }