Radial Sizes and Expansion Behavior of ICMEs in Solar Cycles 23 and 24

Mishra, Wageesh; Doshi, Urmi Vishal; Srivastava, Nandita

doi:10.3389/fspas.2021.713999

Cited by 6 publications

(4 citation statements)

References 98 publications

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“…Similarly, the average P th + P mag inside near-Earth MCs is greater than that in the solar wind background ( § 4.3). These conclusions are broadly consistent with the findings of Gopalswamy et al (2015) and Mishra, Doshi, and Srivastava (2021). 3.…”

Section: Conclusion and Discussionsupporting

confidence: 91%

Characterizing the specific energy and pressure in near-Earth magnetic clouds

Bhattacharjee

Subramanian

Vourlidas

et al. 2023

A&A

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Context. The pressure and energy density of the gas and magnetic field inside solar coronal mass ejections (in relation to that in the ambient solar wind) is thought to play an important role in determining their dynamics as they propagate through the heliosphere. Aims. We compare the specific energy (erg g −1 ), comprising kinetic (H k ), thermal (H th ) and magnetic field (H mag ) contributions, inside magnetic clouds (MCs) and the solar wind background. We examine whether the excess thermal + magnetic pressure and specific energy inside MCs (relative to the background) are correlated with their propagation and internal expansion speeds. We consider whether the excess thermal + magnetic specific energy inside MCs might cause them to resemble rigid bodies in the context of aerodynamic drag. Methods. We used near-Earth in situ data from the WIND spacecraft to identify a sample of 152 well-observed interplanetary coronal mass ejections and their MC counterparts. We compared various metrics based on these data to address our questions.Results. We find that the total specific energy (H) inside MCs is approximately equal to that in the background solar wind. We find that the excess (thermal + magnetic) pressure and specific energy are not well correlated with the near-Earth propagation and expansion speeds. We find that the excess thermal+magnetic specific energy is greater or equivalent to the specific kinetic energy of the solar wind incident in 81-89 % of the MCs we study. This might explain how MCs retain their structural integrity and resist deformation by the solar wind bulk flow.

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Section: Conclusion and Discussionsupporting

confidence: 91%

Characterizing the specific energy and pressure in near-Earth magnetic clouds

Bhattacharjee

Subramanian

Vourlidas

et al. 2023

A&A

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“…As a CME propagates through the inner heliosphere, it may undergo changes in its dynamics and morphology due to its interaction with the ambient SW. Variations in the properties of the ambient SW, such as its speed and density, can result in alterations to the properties of the CME and its shock (Mishra et al 2021;Winslow et al 2021). Investigating the interaction between CMEs and SW, especially in the presence of HSS and SIRs or CIRs, can be accomplished by comparing two scenarios in which an identical CME passes in the presence and absence of them.…”

Section: Methods To Study Cme-sw Interactionmentioning

confidence: 99%

SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind

Mayank,

Vaidya,

Mishra

et al. 2023

ApJS

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Coronal mass ejections (CMEs) are primary drivers of space weather, and studying their evolution in the inner heliosphere is vital to prepare for a timely response. Solar wind streams, acting as background, influence their propagation in the heliosphere and associated geomagnetic storm activity. This study introduces SWASTi-CME, a newly developed MHD-based CME model integrated into the Space Weather Adaptive SimulaTion (SWASTi) framework. It incorporates a nonmagnetized elliptic cone and a magnetized flux rope CME model. To validate the model’s performance with in situ observation at L1, two Carrington rotations were chosen: one during solar maxima with multiple CMEs, and one during solar minima with a single CME. The study also presents a quantitative analysis of CME–solar wind interaction using this model. To account for ambient solar wind effects, two scenarios of different complexity in solar wind conditions were established. The results indicate that ambient conditions can significantly impact some of the CME properties in the inner heliosphere. We found that the drag force on the CME front exhibits a variable nature, resulting in asymmetric deformation of the CME leading edge. Additionally, the study reveals that the impact on the distribution of CME internal pressure primarily occurs during the initial stage, while the CME density distribution is affected throughout its propagation. Moreover, regardless of the ambient conditions, it was observed that, after a certain propagation time (t), the CME volume follows a nonfractal power-law expansion (∝t 3.03−3.33) due to the attainment of a balanced state with ambient.

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“…For instance, the only independent variable V lat had an R 2 a of 0.622, but when the V f rt was added, the R 2 a increased to 0.830. It can be inferred that the front expansion affects the propagation speed of the CME [Mishra et al (2021)]. It was observed that the V sw had no or weak association with the V p .…”

Section: The Relationship Between the Dependent And The Independent P...mentioning

confidence: 99%

Beyond Lateral Expansion: A Multi-parameter Regression-based Model for Inferring Radial Propagation Speeds and Transit Time of Coronal Mass Ejections

Kyeremateng,

Hamadab,

Elsaidd

et al. 2024

Preprint

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Coronal mass ejections (CMEs) have an important kinematic parameter: the propagation speed (Vp), which can be used to determine the transit time of Earth-directed CMEs. This study examines the association between the propagation speed (Vp) and the expansion speeds of 183 interplanetary coronal mass ejections (ICMEs) from 2009 to 2023. We used multiple regression analyses to demonstrate that the Vp of the ICME may be inferred from more than the lateral expansion speed (Vlat). Four regression-based model (RGBM) equations were derived using the solar wind speed (Vsw), the angular width (AW), bulk expansion (Vblk), front expansion (Vfrt), and lateral expansion (Vlat) speeds of the CME to estimate both the Vp and transit times of near-Earth-directed ICMEs/shock. A total of 28 halo ICMEs were used to validate RGBM equations. The most accurate calculation yielded a 6.43-hour mean absolute error (MAE). A feed-forward neural network (FFNN) model was used to estimate the transit times of the 28 halo ICMEs, with an observed MAE of 4.56 hrs. The propagation speed of the RGBM equations that produced the lowest MAE was incorporated into the drag-based model (DBM) to determine the transit times of ICMEs/shocks. The MAE associated with the DBM was found to be 6.03 hrs.

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Radial Sizes and Expansion Behavior of ICMEs in Solar Cycles 23 and 24

Cited by 6 publications

References 98 publications

Characterizing the specific energy and pressure in near-Earth magnetic clouds

Characterizing the specific energy and pressure in near-Earth magnetic clouds

SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind

Beyond Lateral Expansion: A Multi-parameter Regression-based Model for Inferring Radial Propagation Speeds and Transit Time of Coronal Mass Ejections

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