Some Problems of Identifying Types of Large-Scale Solar Wind and Their Role in Magnetosphere Physics: 3. Use of Publishe
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Problems of Identifying Types of Large-Scale Solar Wind and Their Role in Magnetosphere Physics: 3. Use of Published Incorrect Data I. G. Lodkinaa, *, Yu. I. Yermolaeva, **, M. Yu. Yermolaeva, M. O. Riazantsevaa, and A. A. Khokhlacheva aSpace
Research Institute, Russian Academy of Sciences, Moscow, 117997 Russia. *e-mail: [email protected] **e-mail: [email protected]
Received September 2, 2019; revised February 6, 2020; accepted March 5, 2020
Abstract—This paper is a continuation of our works [1, 2], in which we discussed some incorrect approaches to identifying large-scale types of solar wind and related incorrect conclusions drawn when analyzing the solar-terrestrial physics data. In this paper, we analyze the sets of CME-induced, CIR-induced, and multistep magnetic storms for the period of 1996–2004 from the list by Kataoka and Miyoshi [3]. It is shown that a significant number of the events in this list were identified incorrectly and that their interpretation differs, both from our catalog (Yermolaev et al. [4], ftp://ftp.iki.rssi.ru/pub/omni/) for the Sheath, ICME, and CIR and from the catalog by Richardson and Cane [5] for ICME. The use of the uncorrected list of Kataoka and Miyoshi leads to incorrect identification of the interplanetary drivers of magnetic storms and to erroneous conclusions, for example, in paper [6]. DOI: 10.1134/S001095252005007X
1. INTRODUCTION One promising direction of studying the Earth’s magnetosphere response to solar wind (SW) variations is the use of various types of SW phenomena as a kind of interplanetary tracers, which allows one to separate, from the variety of interactions, several, most often repeated scenarios and to establish possible regularities for them. The main large-scale interplanetary SW types that can contain the southward component of the interplanetary magnetic field (IMF) and excite magnetospheric disturbances (see, e.g., [7]) fall into four kinds of phenomena. They are (1) the compression region at the boundary of slow and fast SW flows, the Corotating Interaction Region (CIR); (2, 3) interplanetary manifestations of coronal mass ejections, the ICME including magnetic clouds (MC) and Ejecta; and (4) compression regions in front of the fast ICME, the Sheath, as well as their conventional combinations with direct and reverse shocks (see, for more detail, the characteristics of these phenomena, for example, in papers [8, 9]). This approach allowed us to obtain new and interesting results (see, for example, some recent works [10–13]. At the same time, the number of cases of incorrect identification of SW types is growing in the literature. In some cases, such incorrect identifications of interplanetary drivers can lead to incorrect interpretation of data and to erroneous conclusions [1, 2]. Incorrect
identifications can be conventionally subdivided into two groups. The first group of works uses incorrect criteria, and the erroneous interpretation of such cases is obvious (for example, [14]). In the second group, so-called “CME-induced” phenomena are consid
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