Study of the solar wind coupling to the time difference horizontal geomagnetic field
(2005) In Annales Geophysicae 23(5). p.1949-1957- 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 10-min root-mean-square (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 10-min 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 10-min root-mean-square (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 10-min 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 Y-directions, respectively, at UPS. The most important inputs to the models are the 10-min averages of the solar wind magnetic field component B, and velocity V, and the 10-min 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:
https://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
- 1432-0576
- language
- English
- LU publication?
- yes
- id
- a4d3cbfa-e587-4a27-9779-0b79ff633c25 (old id 225108)
- alternative location
- http://www.ann-geophys.net/23/1949/2005/angeo-23-1949-2005.pdf
- date added to LUP
- 2016-04-01 12:34:42
- date last changed
- 2024-02-24 13:09:31
@article{a4d3cbfa-e587-4a27-9779-0b79ff633c25, 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 10-min root-mean-square (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 10-min 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 Y-directions, respectively, at UPS. The most important inputs to the models are the 10-min averages of the solar wind magnetic field component B, and velocity V, and the 10-min standard deviation of the proton number density a,. The average proton number density n has no influence.}}, author = {{Wintoft, Peter}}, issn = {{1432-0576}}, keywords = {{rapid time variations; geomagnetism and paleomagnetism; magnetosphere interactions; Magnetospheric physics; Solar wind}}, language = {{eng}}, number = {{5}}, pages = {{1949--1957}}, publisher = {{European Geosciences Union}}, series = {{Annales Geophysicae}}, title = {{Study of the solar wind coupling to the time difference horizontal geomagnetic field}}, url = {{http://www.ann-geophys.net/23/1949/2005/angeo-23-1949-2005.pdf}}, volume = {{23}}, year = {{2005}}, }