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<p>Radiation and high-energy particles linked to solar activity around sunspots, including solar flares&#xa0;and coronal mass ejections (CMEs), can be harmful to living organisms. Major geomagnetic storms (GSs) might weaken the geomagnetic field, allowing energetic particles to penetrate the Earth's magnetosphere. Thus, analyzing corresponding solar flares or CMEs provides geoeffective parameters that help in predicting GSs. The purpose of the present study is to compare the geoeffectiveness of interplanetary features associated with DH type II burst-linked Halo CMEs (DH-HCMEs) and those not associated with DH type II bursts (Non-DH-HCMEs). In this study, it was observed that plasma flow pressure (FP) and flow speed (FS) attain their maximum values either before or during the main phase of the GS for both DH-HCMEs and Non-DH-HCMEs. We observed that the maximum values of FS and FP during solar cycle 23 (SC23), solar cycle 24 (SC24), and solar cycle 25 (SC25) are directly correlated with the lowest value of the Dst index for both DH-HCMEs and Non-DH-HCMEs. The analysis further showed that the Dst index decreases more significantly with increasing maximum solar wind speed (Vmax) of the disturbance across all three solar cycles, for moderate, intense, and severe GSs. Additionally, the Vmax associated with DH-HCMEs was consistently higher than that of Non-DH-HCMEs. We found that storm intensity is primarily driven by FP, with higher FP resulting in a more negative Dst index. Different FS regimes were also observed to have&#xa0;an&#xa0;impact&#xa0;on&#xa0;the&#xa0;value of the Dst&#xa0;index. In particular, during DH-HCME events in 2001 and 2005, we noted that when the Dst index rapidly dropped to its minimum—indicating a high rate of change of Dst index—FP did not decrease but instead remained relatively stable at a higher value. Since 2001 and 2005 were highly active years in SC23, the enhanced solar activity likely contributed to the occurrence of more energetic and faster Halo CMEs.</p>

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A comparative study of the geoeffectiveness of interplanetary features of DH-HCMEs and non-DH-HCMEs

  • 期刊论文

  • 发表日期：

    2026年2月23日

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  • Suman Garia,
  • Lalit Garia

摘要

Radiation and high-energy particles linked to solar activity around sunspots, including solar flares and coronal mass ejections (CMEs), can be harmful to living organisms. Major geomagnetic storms (GSs) might weaken the geomagnetic field, allowing energetic particles to penetrate the Earth's magnetosphere. Thus, analyzing corresponding solar flares or CMEs provides geoeffective parameters that help in predicting GSs. The purpose of the present study is to compare the geoeffectiveness of interplanetary features associated with DH type II burst-linked Halo CMEs (DH-HCMEs) and those not associated with DH type II bursts (Non-DH-HCMEs). In this study, it was observed that plasma flow pressure (FP) and flow speed (FS) attain their maximum values either before or during the main phase of the GS for both DH-HCMEs and Non-DH-HCMEs. We observed that the maximum values of FS and FP during solar cycle 23 (SC23), solar cycle 24 (SC24), and solar cycle 25 (SC25) are directly correlated with the lowest value of the Dst index for both DH-HCMEs and Non-DH-HCMEs. The analysis further showed that the Dst index decreases more significantly with increasing maximum solar wind speed (Vmax) of the disturbance across all three solar cycles, for moderate, intense, and severe GSs. Additionally, the Vmax associated with DH-HCMEs was consistently higher than that of Non-DH-HCMEs. We found that storm intensity is primarily driven by FP, with higher FP resulting in a more negative Dst index. Different FS regimes were also observed to have an impact on the value of the Dst index. In particular, during DH-HCME events in 2001 and 2005, we noted that when the Dst index rapidly dropped to its minimum—indicating a high rate of change of Dst index—FP did not decrease but instead remained relatively stable at a higher value. Since 2001 and 2005 were highly active years in SC23, the enhanced solar activity likely contributed to the occurrence of more energetic and faster Halo CMEs.