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Modeling the time behavior of the D st index during the main phase of magnetic storms generated by various types of solar wind

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Results of modeling the time behavior of the D st index at the main phase of 93 geomagnetic storms (−250 < D st ≤ −50 nT) caused by different types of solar wind (SW) streams: magnetic clouds (MC, 10 storms), corotating interaction regions (CIR, 31 storms), the compression region before interplanetary coronal ejections (Sheath before ICME, 21 storms), and “pistons” (Ejecta, 31 storms) are presented. The “Catalog of Large-Scale Solar Wind Phenomena during 1976–2000” (ftp://ftp.iki.rssi.ru/pub/omni/) created on the basis of the OMNI database was the initial data for the analysis. The main phase of magnetic storms is approximated by a linear dependence on the main parameters of the solar wind: integral electric field sumEy, dynamic pressure P d , and fluctuation level sB in IMF. For all types of SW, the main phase of magnetic storms is better modeled by individual values of the approximation coefficients: the correlation coefficient is high and the standard deviation between the modeled and measured values of D st is low. The accuracy of the model in question is higher for storms from MC and is lower by a factor of ∼2 for the storms from other types of SW. The version of the model with the approximation coefficients averaged over SW type describes worse variations of the measured D st index: the correlation coefficient is the lowest for the storms caused by MC and the highest for the Sheath- and CIR-induced storms. The model accuracy is the highest for the storms caused by Ejecta and, for the storms caused by Sheath, is a factor of ∼1.42 lower. Addition of corrections for the prehistory of the development of the beginning of the main phase of the magnetic storm improves modeling parameters for all types of interplanetary sources of storms: the correlation coefficient varies within the range from r = 0.81 for the storms caused by Ejecta to r = 0.85 for the storms caused by Sheath. The highest accuracy is for the storms caused by MC. It is, by a factor of ∼1.5, lower for the Sheath-induced storms.

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  1. Space Research Institute, Russian Academy of Sciences, ul. Profsoyuznaya 84/32, Moscow, 117997, Russia

    N. S. Nikolaeva, Yu. I. Yermolaev & I. G. Lodkina

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  1. N. S. Nikolaeva
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  2. Yu. I. Yermolaev
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Original Russian Text © N.S. Nikolaeva, Yu.I. Yermolaev, I.G. Lodkina, 2013, published in Kosmicheskie Issledovaniya, 2013, Vol. 51, No. 6, pp. 443–454.

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Nikolaeva, N.S., Yermolaev, Y.I. & Lodkina, I.G. Modeling the time behavior of the D st index during the main phase of magnetic storms generated by various types of solar wind. Cosmic Res 51, 401–412 (2013). https://doi.org/10.1134/S0010952513060038

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