Propagation of coronal mass ejections from the Sun to the Earth

Mishra, Wageesh; Teriaca, L.

doi:10.1007/s12036-023-09910-6

Cited by 9 publications

(3 citation statements)

References 313 publications

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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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Section: Introductionmentioning

confidence: 99%

Hemispheric Distribution of Halo Coronal Mass Ejection Source Locations

Zhang,

Deng,

Deng

et al. 2024

ApJ

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“…Space weather forecasting is necessary because these materials and magnetic fluxes can even generate currents within the Earth's crust that cause severe electrical damage to installations (Pirjola 2005). The key to space weather forecasting lies in clarifying the early evolution of CMEs, such as their initiation and dynamics processes (e.g., Mishra & Teriaca 2023). Typically, CMEs exhibit a classic threecomponent structure (Illing & Hundhausen 1985;Shen et al 2012b;Carley et al 2012;Song et al 2023) that appears in the outer corona as a bright front, followed by a darker cavity that frequently contains a bright core, with typical angular widths around 50°-60° (Gopalswamy et al 2014;Pant et al 2021).…”

Section: Introductionmentioning

confidence: 99%

On the Determining Physical Factor of Jet-related Coronal Mass Ejections’ Morphology in the High Corona

Duan,

Shen,

Tang

et al. 2024

ApJ

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A solar jet can often cause coronal mass ejections (CMEs) with different morphologies in the high corona, for example, jet-like CMEs, bubble-like CMEs, and so-called twin CMEs that include a pair of simultaneous jet-like and bubble-like CMEs. However, what determines the morphology of a jet-related CME is still an open question. Using high spatiotemporal resolution stereoscopic observations taken by the Solar Dynamics Observatory and the Solar Terrestrial Relations Observatory from 2010 October to 2012 December, we performed a statistical study of jet-related CMEs to study the potential physical factors that determine the morphology of CMEs in the outer corona. Our statistical sample includes 16 jet-related CME events of which seven are twin CME events and nine are jet-like narrow CMEs. We find that all CMEs in our sample were accompanied by filament-driven blowout jets and Type III radio bursts during their initial formation and involved magnetic reconnection between filament channels and the surrounding magnetic fields. Most of our cases occurred in a fan-spine magnetic configuration. Our study suggests that the bubble-like components of twin CMEs lacking an obvious core are related to the expansion of the closed-loop systems next to the fan-spine topology, while the jet-like component is from the coronal extension of the jet plasma along open fields. Based on the statistical results, we conclude that the morphology of jet-related CMEs in the high corona may be related to the filament length and the initial magnetic null point height of the fan-spine structures.

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“…Further, due to the sparse distribution of in situ spacecraft, it is difficult for multiple spacecraft to become coaligned to measure the thermal state of the same ICME at different distances (Phillips et al 1995;Winslow et al 2021). It is often challenging to associate the remote sensing observations of global structures of CMEs with their local in situ observations (Mishra & Srivastava 2013;Mishra & Teriaca 2023). Most of the routine coronagraphic observations of CMEs are in white light, which does allow continuous tracking of density-enhanced structures, but lacks any thermodynamic information.…”

Section: Introductionmentioning

confidence: 99%

Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections

Khuntia,

Mishra,

Mishra

et al. 2023

ApJ

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Coronal mass ejections (CMEs) are the most energetic expulsions of magnetized plasma from the Sun that play a crucial role in space weather dynamics. This study investigates the diverse kinematics and thermodynamic evolution of two CMEs (CME1: 2011 September 24 and CME2: 2018 August 20) at coronal heights where thermodynamic measurements are limited. The peak 3D propagation speed of CME1 is high (1885 km s−1) with two-phase expansion (rapid and nearly constant), while the peak 3D propagation speed of CME2 is slow (420 km s−1) with only a gradual expansion. We estimate the distance-dependent variations in the polytropic index, heating rate, temperature, and internal forces implementing the revised FRIS model, taking inputs of 3D kinematics estimated from the graduated cylindrical shell model. We find CME1 exhibiting heat release during its early-rapid acceleration decrease and jumps to the heat-absorption state during its constant acceleration phase. In contrast to CME1, CME2 shows a gradual transition from the near-adiabatic to the heat-absorption state during its gradually increasing acceleration. Our analysis reveals that although both CMEs show differential heating, they experience heat absorption during their later propagation phases, approaching the isothermal state. The faster CME1 achieves an adiabatic state followed by an isothermal state at smaller distances from the Sun than the slower CME2. We also find that the expansion of CMEs is primarily influenced by centrifugal and thermal pressure forces, with the Lorentz force impeding expansion. Multiwavelength observations of flux-ropes at source regions support the FRIS-model-derived findings at initially observed lower coronal heights.

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Propagation of coronal mass ejections from the Sun to the Earth

Cited by 9 publications

References 313 publications

Hemispheric Distribution of Halo Coronal Mass Ejection Source Locations

Hemispheric Distribution of Halo Coronal Mass Ejection Source Locations

On the Determining Physical Factor of Jet-related Coronal Mass Ejections’ Morphology in the High Corona

Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections

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