Parameters which influence efficiency of geomagnetically induced currents generation by non-storm Pc5-6/Pi3 geomagnetic pulsations

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We studied geomagnetic pulsations with periods of about several minutes and geomagnetically induced currents related to them. The interrelation is studied between efficiency of pulsations in currents’ generation and parameters of interplanetary magnetic field and plasma of the solar wind at different delays. Geomagnetic data and the recordings of geomagnetically induced currents in the Russian North and Finland are used for the analysis. It is shown that efficiency of current generation by pulsations grows if the solar wind velocity is not lower than 500 km/s for several hours.

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作者简介

Ya. Sakharov

Polar Geophysical Institute; Geophysical Center of the Russian Academy of Sciences

Email: nyagova@ifz.ru
俄罗斯联邦, Apatity; Moscow

N. Yagova

Geophysical Center of the Russian Academy of Sciences; Schmidt Institute of Physics of the Earth of the Russian Academy of Sciences

编辑信件的主要联系方式.
Email: nyagova@ifz.ru
俄罗斯联邦, Moscow; Moscow

V. Bilin

Polar Geophysical Institute

Email: nyagova@ifz.ru
俄罗斯联邦, Apatity

V. Selivanov

Northern Energetics Research Center, Kola Science Center of the Russian Academy of Sciences

Email: nyagova@ifz.ru
俄罗斯联邦, Apatity

T. Aksenovich

Northern Energetics Research Center, Kola Science Center of the Russian Academy of Sciences

Email: nyagova@ifz.ru
俄罗斯联邦, Apatity

V. Pilipenko

Geophysical Center of the Russian Academy of Sciences; Schmidt Institute of Physics of the Earth of the Russian Academy of Sciences

Email: nyagova@ifz.ru
俄罗斯联邦, Moscow; Moscow

参考

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2. Fig. 1. Dependence of the solar wind speed V averaged over the intervals at which the GIT oscillation spread ∆I > 10 A depends on the averaging time τ for two groups of pulsations with different RIB ratios. The solid lines show the results for the entire observation period (2014-2018), while the dashed and dashed lines show the results for two-year subsamples. The horizontal dashed line shows the average V value for the entire observation period

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3. Fig. 2. Distributions with respect to the RIB ratio for high (upper panels) and low (lower panels) solar wind speeds of suprathreshold GIT recording intervals for two threshold values: ∆I = 2 A (a, b) and ∆I = 10 A (c, d). Threshold values: V = 475 km/s, τ = 8 h

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4. Fig. 3. Dependence on solar wind speed V and averaging time τ of the fraction of intervals with GIT-effective pulsations P(RIB > Rb) in the total number of intervals for which pulsation-related GITs with ∆I > 10 A were observed

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