An Insight into the Coupling of CME Kinematics in Inner and Outer Corona and the Imprint of Source Regions

Majumdar, Satabdwa; Patel, Ritesh; Pant, Vaibhav; Banerjee, D.

doi:10.3847/1538-4357/ac1592

Cited by 11 publications

(11 citation statements)

References 41 publications

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“…The initial rapid expansion of volume can be attributed to the rapid angular width expansion in the inner corona as was recently reported by Cremades et al (2020) and Majumdar et al (2020), while it seems the relatively slower volume expansion of CMEs in the outer corona might be a consequence of the total pressure difference in the inside and outside of the CME. These results thus strongly indicate how the kinematic properties of CMEs in the inner corona are strikingly different from the properties in the outer corona, lending support to the recent report by Majumdar et al (2021b). It is also worthwhile to note the significance of the inclusion of K-Cor data along with the COR-1 data in order to arrive at these results.…”

Section: Evolution Of Modelled Cme Volumesupporting

confidence: 83%

On the Variation of Volumetric Evolution of CMEs from Inner to Outer Corona

Majumdar,

Patel,

Pant

2022

Preprint

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Some of the major challenges faced in understanding the early evolution of Coronal Mass Ejections (CMEs) are due to limited observations in the inner corona (< 3 R ) and the plane of sky measurements. In this work, we have thus extended the application of the Graduated Cylindrical Shell (GCS) model to the inner coronal observations from the ground-based coronagraph K-Cor of the Mauna Loa Solar Observatory (MLSO) along with the pair of observations from COR-1 onboard the Solar Terrestrial Relations Observatory (STEREO). We study the rapid initial acceleration and width expansion phase of 5 CMEs in white-light in the lower heights. We also study the evolution of the modelled volume of these CMEs in inner corona and report for the first time, a power law dependence of the CME volume with distance from the Sun. We further find the volume of ellipsoidal leading front and the conical legs follow different power laws, thus indicating differential volume expansion through a CME. The study also reveals two distinct power laws for the total volume evolution of CMEs in the inner and outer corona, thus suggesting different expansion mechanisms at these different heights. These results besides aiding our current understanding on CME evolution, will also provide better constraints to CME initiation and propagation models. Also, since the loss of STEREO-B (and hence COR-1B data) from 2016, this modified GCS model presented here will still enable stereoscopy in the inner corona for the 3D study of CMEs in white-light.

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Section: Evolution Of Modelled Cme Volumesupporting

confidence: 83%

On the Variation of Volumetric Evolution of CMEs from Inner to Outer Corona

Majumdar,

Patel,

Pant

2022

Preprint

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“…Webb et al, 2000;Zhao et al, 2017). Here, we demonstrate how the speed and width distributions (Figures 6 and 7) of CMEs change when they are separated into three broad categories: AR eruption (Majumdar et al, 2021;Pal et al, 2018), PE (R. Munro et al, 1979;Sheeley et al, 1980;St. Cyr et al, 1999;D.…”

Section: Effect Of Source Region On the Speed And Width Distributionssupporting

confidence: 56%

Correcting Projection Effects in CMEs Using GCS‐Based Large Statistics of Multi‐Viewpoint Observations

Gandhi,

Patel,

Pant

et al. 2024

Space Weather

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This study addresses the limitations of single‐viewpoint observations of Coronal Mass Ejections (CMEs) by presenting results from a 3D catalog of 360 CMEs during solar cycle 24, fitted using the Graduated Cylindrical Shell (GCS) model. The data set combines 326 previously analyzed CMEs and 34 newly examined events, categorized by their source regions into active region (AR) eruptions, active prominence (AP) eruptions, and prominence eruptions (PE). Estimates of errors are made using a bootstrapping approach. The findings highlight that the average 3D speed of CMEs is ∼1.3 times greater than the 2D speed. PE CMEs tend to be slow, with an average speed of 432 km s−1. AR and AP speeds are higher, at 723 and 813 km s−1, respectively, with the latter having fewer slow CMEs. The distinctive behavior of AP CMEs is attributed to factors like overlying magnetic field distribution or geometric complexities leading to less accurate GCS fits. A linear fit of projected speed to width gives a gradient of ∼2 km s−1 deg−1, which increases to 5 km s−1 deg−1 when the GCS‐fitted ‘true’ parameters are used. Notably, AR CMEs exhibit a high gradient of 7 km s−1 deg−1, while AP CMEs show a gradient of 4 km s−1 deg−1. PE CMEs, however, lack a significant speed‐width relationship. We show that fitting multi‐viewpoint CME images to a geometrical model such as GCS is important to study the statistical properties of CMEs, and can lead to a deeper insight into CME behavior that is essential for improving future space weather forecasting.

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“…(2) between A R,max and V R,max , assuming a linear relationship. In a recent study, Majumdar et al (2021a) derived kinematic properties of CMEs using the GCS approach. In particular, they also derived the relationship between A max and V max (of the CMEs).…”

Section: Summary and Discussionmentioning

confidence: 99%

Parametric study of the kinematic evolution of coronal mass ejection shock waves and their relation to flaring activity

Jarry

Rouillard

Plotnikov

et al. 2023

A&A

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Context. Coronal and interplanetary shock waves produced by coronal mass ejections (CMEs) are major drivers of space-weather phenomena, inducing major changes in the heliospheric radiation environment and directly perturbing the near-Earth environment, including its magnetosphere. A better understanding of how these shock waves evolve from the corona to the interplanetary medium can therefore contribute to improving nowcasting and forecasting of space weather. Early warnings from these shock waves can come from radio measurements as well as coronagraphic observations that can be exploited to characterise the dynamical evolution of these structures. Aims. Our aim is to analyse the geometrical and kinematic properties of 32 CME shock waves derived from multi-point white-light and ultraviolet imagery taken by the Solar Dynamics Observatory (SDO), Solar and Heliospheric Observatory (SoHO), and Solar-Terrestrial Relations Observatory (STEREO) to improve our understanding of how shock waves evolve in 3D during the eruption of a CME. We use our catalogue to search for relations between the shock wave’s kinematic properties and the flaring activity associated with the underlying genesis of the CME piston. Methods. Past studies have shown that shock waves observed from multiple vantage points can be aptly reproduced geometrically by simple ellipsoids. The catalogue of reconstructed shock waves provides the time-dependent evolution of these ellipsoidal parameters. From these parameters, we deduced the lateral and radial expansion speeds of the shocks evolving over time. We compared these kinematic properties with those obtained from a single viewpoint by SoHO in order to evaluate projection effects. Finally, we examined the relationships between the shock wave and the associated flare when the latter was observed on the disc by considering the measurements of soft and hard X-rays. Results. We find that at around 25 solar radii (R⊙), the shape of a shock wave is very spherical, with a ratio between the lateral and radial dimensions (minor radii) remaining at around b/a ≈ 1.03 and a radial to lateral speed ratio (VR/VL)≈1.44. The CME starts to slow down a few tens of minutes after the first acceleration and then propagates at a nearly constant speed. We revisit past studies that show a relation between the CME speed and the soft X-ray emission of the flare measured by the Geostationary Operational Environmental Satellite (GOES) and extend them to higher flare intensities and shock speeds. The time lag between the peak of the flare and of the CME speed is up to a few tens of minutes. We find that for several well-observed shock onsets, a clear correlation is visible between the derivative of the soft X-ray flux and the acceleration of the shock wave.

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An Insight into the Coupling of CME Kinematics in Inner and Outer Corona and the Imprint of Source Regions

Cited by 11 publications

References 41 publications

On the Variation of Volumetric Evolution of CMEs from Inner to Outer Corona

On the Variation of Volumetric Evolution of CMEs from Inner to Outer Corona

Correcting Projection Effects in CMEs Using GCS‐Based Large Statistics of Multi‐Viewpoint Observations

Parametric study of the kinematic evolution of coronal mass ejection shock waves and their relation to flaring activity

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