Nature and Variability of the Electron Velocity Distribution Functions and the Nonequilibrium Boltzmann Entropy in the Solar Wind at the First Lagrangian (L1) Point During the Halo CME Event on 25 July 2004

Nampoothiri, Govind G.; Thampi, R. Satheesh; Thampi, Smitha V.; Pant, Tarun Kumar; Abhishek, J. K.

doi:10.1007/s11207-021-01900-7

Cited by 1 publication

(1 citation statement)

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“…HCMEs are an energetic subset (Gopalswamy et al 2010b) of coronal mass ejections (CMEs) that have considerable heliospheric effects, have profound impacts on space weather (Michalek et al 2006(Michalek et al , 2007, and are a significant contributor to powerful geomagnetic storms (Webb et al 2000;Michalek et al 2008;Kwon et al 2015;Temmer 2021). In particular, the Sun's front-side HCMEs (which can tag source locations) as observed from the Earth have direct geoeffectiveness for the solar-terrestrial relationship (Zhao & Webb 2003;Shen et al 2014;Lee et al 2015;Scolini et al 2018;Nampoothiri et al 2021;Shanmugaraju et al 2021;Gopalswamy et al 2023;Mishra & Teriaca 2023). A considerable number of HCMEs have been detected by the Large Angle and Spectrometric Coronagraph Experiment (LASCO) C2 and C3 telescopes (Brueckner et al 1995) on the Solar and Heliospheric Observatory (SOHO) (Domingo et al 1995), which have given us more opportunity to examine the temporal variation of HCMEs.…”

Section: Introductionmentioning

confidence: 99%

Hemispheric Distribution of Halo Coronal Mass Ejection Source Locations

Zhang,

Deng,

Deng

et al. 2024

ApJ

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The hemispheric asymmetry of solar activity is one of the essential physical consequences of the interior dynamo process. However, the hemispheric distribution of halo coronal mass ejection (HCME) source locations has not been investigated in detail. Based on the HCME catalog identified from the Large Angle and Spectrometric Coronagraph Experiment on board the Solar and Heliospheric Observatory, we perform a hemispheric distribution analysis of the HCME source locations from 1996 April to 2022 June. The main results are as follows. (1) The HCME source locations are confined to the active region belt, and there is no “rush to the poles” phenomenon that is unique to large-scale magnetic activity. (2) The HCME source locations exhibit a general hemispheric asymmetry, and autoregressive moving-average model results show that the asymmetry of HCME source locations is significantly different from that of sunspot activity. (3) The hemispheric distribution of cycle 24 is different from that of cycle 23, potentially as a result of the heliospheric dynamic pressure having noticeably decreased after the polarity reversal of cycle 23. Our results contribute to a more comprehensive understanding of the hemispheric asymmetry of energetic magnetic structures and give a new perspective on understanding the geoeffectiveness of HCMEs.

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