Formation of Coronal Mass Ejections in the Solar Corona and Propagation of the Resulting Plasma Streams in the Heliosphe
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E PLASMA
Formation of Coronal Mass Ejections in the Solar Corona and Propagation of the Resulting Plasma Streams in the Heliosphere V. A. Slemzina, *, F. F. Goryaeva, D. G. Rodkina, Yu. S. Shugayb, and S. V. Kuzina a
b
P.N. Lebedev Physical Institute, Russian Academy of Sciences, Moscow, 119991 Russia Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, 119991 Russia *e-mail: [email protected] Received December 5, 2018; revised March 20, 2019; accepted March 25, 2019
Abstract—A review of studies of coronal mass ejections (CMEs) and the propagation of the resulting interplanetary coronal mass ejections (ICMEs) in the heliosphere is presented. The main parameters of ICMEs, their differences from other types of solar wind (SW) streams, and correlation of the ICME occurrence rate with the state of solar activity are considered. Special attention is paid to the formation and simulation of the ion composition of the CME/ICME plasma, which is one of the key factors in identifying the types and sources of SW streams, especially in complex structures formed in the heliosphere during the interaction of streams. Models for predicting the parameters of SW streams from observational data are considered. The review also presents the lists of literature sources on coronal ejections and databases on the parameters of SW streams, as well as numerous references to the works on the phenomena under study. DOI: 10.1134/S1063780X19100076
1. INTRODUCTION. TYPES OF SOLAR WIND STREAMS Measurements of the parameters of solar wind (SW) in the near-Earth and interplanetary space, which have been performed for more than half a century, demonstrate both long-term variations associated with solar activity cycles and short-term periodic and nonperiodic changes caused by the variability of SW sources. Large-scale SW streams are divided into slow and fast (high-speed) ones, depending on their velocity, which are recorded in situ (i.e., directly in the SW stream) by using probes installed onboard spacecraft. SW streams with velocities of lower than 400– 450 km/s (see, e.g., [1]) are considered slow, while those with velocities of higher than 450–500 km/s are considered fast. Sometimes, SW streams with velocities of higher than 725 km/s are called superfast ones [2]. The average velocity, density, and temperature of SW protons vary from cycle to cycle and are related to the level of solar activity. As an example, Table 1 presents the average values of the velocity, density, and temperature of SW protons for the growth phases of the 22nd (1986–1989), 23rd (1996–2000), and 24th (2009–2014) solar cycles [3]. The SW proton flux at a distance of 1 AU from the Sun, averaged over a long period of time, varies from 2 × 108 cm–2 s–1 in the
high-speed components of SW to 4 × 108 cm–2 s–1 in the slow SW [4]. The following types of large-scale streams associated with their main sources in the solar corona can be distinguished in the SW: quasi-steady high-speed streams (HSSs) from coronal holes (CHs), heliospheric current sheet (HCS),
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