More than 140 isolated non-recurrent geomagnetic storms (GMSs) of various intensities from extreme to weak are considered; these are reliably identified with solar eruptive sources (coronal mass ejections, CMEs). The analysis aims to obtain a possibly complete picture of the relationship between the transit time of propagation of CMEs and interplanetary coronal mass ejections (ICMEs) from the Sun to the Earth (more precisely, the time interval Δ t p $\Delta t_{p}$ from the moment of an eruption until the peak of the corresponding GMS) and the maximum intensity of this GMS, as measured by the disturbance storm time geomagnetic index Dst. Two groups of events are singled out: one includes GMSs, the source of which was an eruption from an active region (AR events), the other GMSs caused by filament eruptions from quiescent areas of the Sun located outside ARs (QS events). The distribution of the large number of the analyzed events on a Δ t p $\Delta t_{p}$ – Dst plane confirms and substantially clarifies the known regularities. The AR events are characterized by a shorter transit time ( Δ t p ≈ 1 $\Delta t_{p} \approx 1$ –4 days) and much stronger GMSs (Dst up to –600 nT mainly) in comparison with the QS events ( Δ t p ≈ 3 $\Delta t_{p} \approx 3$ –5 days, Dst > –200 nT). For events of both groups, the shorter the transit time of CMEs/ICMEs, the more intense the GMSs; in particular, for AR events when Δ t p $\Delta t_{p}$ declines from 4 to 1 day, Dst decreases on average from –100 to –470 nT and can reach – 900 nT. From the point of view of the nature of GMSs and their sources on the Sun, the obtained results mean that both the speed of CMEs/ICMEs and the strength of the magnetic field transported by them are largely determined by the parameters of the corresponding eruptions, in particular, by the eruptive magnetic flux and the released energy.

中文翻译：

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ICME的渡越时间与始发地磁风暴强度的关系

考虑了 140 多个从极到弱的各种强度的孤立的非周期性地磁暴 (GMS)；这些可以通过太阳爆发源（日冕物质抛射，CME）可靠地识别出来。该分析旨在获得 CME 传播的传播时间与从太阳到地球的行星际日冕物质抛射 (ICME) 之间关系的可能完整图景（更准确地说，时间间隔 Δ tp $\Delta t_{p} $从喷发时刻到相应 GMS 的峰值）和该 GMS 的最大强度，由扰动风暴时间地磁指数 Dst 测量。挑选出两组事件：一组包括 GMS，其来源是活动区域的喷发（AR 事件），由位于 AR 之外的太阳静止区域的细丝喷发引起的其他 GMS（QS 事件）。大量分析事件在 Δtp $\Delta t_{p}$ – Dst 平面上的分布证实并充分阐明了已知规律。与 QS 事件相比，AR 事件的特点是更短的传输时间（Δ tp ≈ 1 $\Delta t_{p} \approx 1$ –4 天）和更强的 GMS（Dst 主要高达 –600 nT）（ Δ tp ≈ 3 $\Delta t_{p} \大约 3$ –5 天，Dst > –200 nT）。对于两组事件，CMEs/ICMEs的传播时间越短，GMSs越强烈；特别是，对于AR事件，当Δtp$\Delta t_{p}$从4天下降到1天时，Dst平均从–100下降到–470 nT，并且可以达到–900 nT。从 GMS 的性质及其在太阳上的来源来看，