Tracking the 3D evolution of a halo coronal mass ejection using the revised cone model

Zhang, Q. M.

doi:10.1051/0004-6361/202142942

Cited by 10 publications

(7 citation statements)

References 85 publications

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“…The revised cone model is developed to track the 3D evolution of filament eruptions or CMEs and investigate the properties of the non-radial filament eruptions or CMEs, which require observations from at least two viewpoints (Zhang 2021(Zhang , 2022. The revised cone model is based on the assumption that the shape of the eruptions or CMEs is the icecream cone, where the cone apex is located at the source regions and the cone base is spheric.…”

Section: Models and Methodsmentioning

confidence: 99%

Simultaneous Horizontal and Vertical Oscillation of a Quiescent Filament Observed by CHASE and SDO

Dai,

Zhang,

Qiu

et al. 2023

ApJ

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In this paper, we present the imaging and spectroscopic observations of the simultaneous horizontal and vertical large-amplitude oscillation of a quiescent filament triggered by an extreme-ultraviolet (EUV) wave on 2022 October 2. Particularly, the filament oscillation involved winking phenomenon in Hα images and horizontal motions in EUV images. Originally, a filament and its overlying loops across AR 13110 and 13113 erupted with a highly inclined direction, resulting in an X1.0 flare and a non-radial coronal mass ejection. The fast lateral expansion of loops excited an EUV wave and the corresponding Moreton wave propagating northward. Once the EUV wave front arrived at the quiescent filament, the filament began to oscillate coherently along the horizontal direction, and the “winking filament” appeared concurrently in Hα images. The horizontal oscillation involved an initial amplitude of ∼10.2 Mm and a velocity amplitude of ∼46.5 km s−1, lasting for ∼3 cycles with a period of ∼18.2 minutes and a damping time of ∼31.1 minutes. The maximum Doppler velocities of the oscillating filament are 18 km s−1 (redshift) and −24 km s−1 (blueshift), which were derived from the spectroscopic data provided by the Chinese Hα Solar Explorer/Hα Imaging Spectrograph. The three-dimensional velocity of the oscillation is determined to be ∼50 km s−1 at an angle of ∼50° to the local photosphere plane. Based on the wave–filament interaction, the minimum energy of the EUV wave is estimated to be 2.7 × 1020 J. Furthermore, this event provides evidence that Moreton waves should be excited by the highly inclined eruptions.

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Section: Models and Methodsmentioning

confidence: 99%

Simultaneous Horizontal and Vertical Oscillation of a Quiescent Filament Observed by CHASE and SDO

Dai,

Zhang,

Qiu

et al. 2023

ApJ

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“…Coronal mass ejections (CMEs) are impulsive, large-scale eruptions of magnetic field and corona plasma into the heliosphere (see Chen 2011;Georgoulis et al 2019, and references therein). A majority of CMEs are produced by eruptions of prominences or magnetic flux ropes originating from quiet regions or active regions (Fan 2005;Aulanier et al 2010;Yan et al 2018;Zhang 2022;Zhou et al 2023). The speeds of CMEs have a wide range from ∼100 km s −1 to ≥3000 km s −1 (Yashiro et al 2004).…”

Section: Introductionmentioning

confidence: 99%

First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops

Zhang

et al. 2022

ApJL

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In this Letter, we perform a detailed analysis of the M5.5 class eruptive flare occurring in active region 12,929 on 2022 January 20. The eruption of a hot channel generates a fast coronal mass ejection (CME) and a dome-shaped extreme-ultraviolet (EUV) wave at speeds of 740–860 km s−1. The CME is associated with a type II radio burst, implying that the EUV wave is a fast-mode shock wave. During the impulsive phase, the flare shows quasi-periodic pulsations (QPPs) in EUV, hard X-ray, and radio wavelengths. The periods of QPPs range from 18 to 113 s, indicating that flare energy is released and nonthermal electrons are accelerated intermittently with multiple timescales. The interaction between the EUV wave and low-lying adjacent coronal loops (ACLs) results in contraction, expansion, and transverse vertical oscillation of ACLs. The speed of contraction in 171, 193, and 211 Å is higher than that in 304 Å. The periods of oscillation are 253 s and 275 s in 304 Å and 171 Å, respectively. A new scenario is proposed to explain the interaction. The equation that interprets the contraction and oscillation of the overlying coronal loops above a flare core can also interpret the expansion and oscillation of ACLs, suggesting that the two phenomena are the same in essence.

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“…When spacecraft at different heliospheric distances are near radially aligned, they have the opportunity to measure the same CME. This makes the case studies and statistical studies of a CME's radial evolution feasible (Burlaga et al 1981;Cane et al 1997;Liu et al 2005Liu et al , 2008Möstl et al 2012;Ruffenach et al 2012;Good et al 2015;Li et al 2017;Wang et al 2018;Good et al 2019;Chi et al 2020Chi et al , 2021Lugaz et al 2020;Salman et al 2020;Davies et al 2021Davies et al , 2022Winslow et al 2021aWinslow et al , 2021bLugaz et al 2022;Möstl et al 2022;Réville et al 2022;Scolini et al 2022;Xu et al 2022;Zhang 2022;Zhao et al 2022). Using combined, multipoint observations of the same magnetic clouds by STEREO-A, STEREO-B, ACE, Wind, and THEMIS, Ruffenach et al (2012) confirmed the occurrence of magnetic cloud erosion during their propagation from the Sun to Earth.…”

Section: Introductionmentioning

confidence: 97%

Global Morphology Distortion of the 2021 October 9 Coronal Mass Ejection from an Ellipsoid to a Concave Shape

Yang

Hou

Feng

et al. 2023

ApJ

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This paper presents a study of a 2021 October 9 coronal mass ejection (CME) with multipoint imaging and in situ observations. We also simulate this CME from the Sun to Earth with a passive tracer to tag the CME’s motion. The coronagraphic images show that the CME is observed as a full halo by SOHO and as a partial halo by STEREO-A. The heliospheric images reveal that the propagation speed of the CME approaches about 1° hr−1, suggesting a slow CME. With simulated results matching these observation results, the simulation discloses that as the CME ejects from the Sun out to interplanetary space, its global morphology is distorted from an ellipsoid to a concave shape owing to interactions with the bimodal solar wind. The cross section of the CME’s flux rope structure transforms from a circular shape into a flat one. As a result of the deflection, the propagation direction of the CME is far away from the Sun–Earth line. This means that the CME flank (or the ICME leg) likely arrives at both Solar Orbiter and the L1 point. From the CME’s eruption to 1 au, its volume and mass increase by about two orders and one order of magnitude, respectively. Its kinetic energy is about 100 times larger than its magnetic energy at 1 au. These results have important implications for our understanding of CMEs’ morphology, as well as their space weather impacts.

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Tracking the 3D evolution of a halo coronal mass ejection using the revised cone model

Cited by 10 publications

References 85 publications

Simultaneous Horizontal and Vertical Oscillation of a Quiescent Filament Observed by CHASE and SDO

Simultaneous Horizontal and Vertical Oscillation of a Quiescent Filament Observed by CHASE and SDO

First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops

Global Morphology Distortion of the 2021 October 9 Coronal Mass Ejection from an Ellipsoid to a Concave Shape

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