Is There a Dynamic Difference between Stealthy and Standard Coronal Mass Ejections?

Bao, Ying; Бемпорад, А.; Li, Feng; Nitta, N.; Gan, Weiqun

doi:10.3847/1538-4357/aca52c

Cited by 3 publications

(2 citation statements)

References 73 publications

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“…3.12 0.85 10 31 ( )  ´erg. Assuming an increment of the CME's mass of ∼10% during its propagation, m CME reaches (1.89 ± 0.52) × 10 15 g, which is close to the mass of the CME front on 2011 September 13 derived by using the WL observation (Ying et al 2023). As a consequence, the kinetic energy of the CME increases to (3.43 ± 0.94) × 10 31 erg, which is 1 order of magnitude higher than that of the HC (Table 2).…”

Section: Energeticssupporting

confidence: 78%

Energetics of a Solar Flare and a Coronal Mass Ejection Generated by a Hot Channel Eruption

Zhang,

Teng,

et al. 2023

ApJ

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Hot channels (HCs) are prevalent in the solar corona and play a critical role in driving flares and coronal mass ejections (CMEs). In this paper, we estimate the energy content of an X1.4 eruptive flare with a fast CME generated by an HC eruption on 2011 September 22. Originating from NOAA Active Region 11302, the HC is the most dramatic feature in 131 and 94 Å images observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). The flare is simultaneously observed by SDO/AIA, the Reuven Ramaty High-energy Solar Spectroscopic Imager, and the Extreme-ultraviolet Imager on board the “behind” Solar Terrestrial Relations Observatory (STEREO). The CME is simultaneously detected by the white-light coronagraphs of the Large Angle Spectroscopic Coronagraph on board the Solar and Heliospheric Observatory and the COR1 coronagraph on board the behind STEREO. Using multiwavelength and multiview observations of the eruption, various energy components of the HC, flare, and CME are calculated. The thermal and kinetic energies of the HC are (1.77 ± 0.61) × 1030 erg and (2.90 ± 0.79) × 1030 erg, respectively. The peak thermal energy of the flare and total radiative loss of the soft X-ray–emitting plasma are (1.63 ± 0.04) × 1031 erg and (1.03–1.31) × 1031 erg, respectively. The ratio between the thermal energies of the HC and flare is 0.11 ± 0.03, suggesting that the thermal energy of the HC is not negligible. The kinetic and potential energies of the CME are (3.43 ± 0.94) × 1031 erg and (2.66 ± 0.49) × 1030 erg, yielding a total energy of (3.69 ± 0.98) × 1031 erg for the CME. Continuous heating of the HC is required to balance the rapid cooling by heat conduction, which probably originates from intermittent magnetic reconnection at the flare current sheet. Our investigation may provide insight into the buildup, release, and conversion of energies in large-scale solar eruptions.

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Section: Energeticssupporting

confidence: 78%

Energetics of a Solar Flare and a Coronal Mass Ejection Generated by a Hot Channel Eruption

Zhang,

Teng,

et al. 2023

ApJ

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“…For these reasons, the velocity distribution of the CS and the post-CME environment surrounding the CS is assumed to be equal to the outflow speed of the blob and uniformly distributed. Statistically, the post-CME speed is expected to be smaller than the measured speed of the CME front of ∼250 km s −1 , as we derived from a comparison between the speeds of the CME core and front measured in a series of slow CME events reported by Ying et al (2023). We obtained that on average the ratio between these two speeds is between 0.3 and 1.5 in a distance range between 1.7 and 3 R e .…”

Section: R T Hmentioning

confidence: 62%

First Determination in the Extended Corona of the 2D Thermal Evolution of a Current Sheet after a Solar Eruption

Bemporad,

Shi,

et al. 2024

ApJ

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For the first time the evolution of the coronal reconfiguration after a coronal mass ejection (CME) was observed by the multichannel Metis Coronagraph on board the ESA–Solar Orbiter mission. The images acquired in visible light (VL) between 3.0 and 5.4 R ⊙ show the formation after a CME of a bright elongated radial feature interpreted as a post-CME current sheet (CS). The unique combination of VL and UV images allowed the time evolution of multiple plasma physical parameters inside and outside the CS region to be mapped in 2D for the first time. The CS electron temperature reached peak values higher than 1 MK, more than twice as high as the surrounding corona. An elongated vertical diffusion region, characterized as a region of much higher thermal pressure and lower magnetic pressure, is observed to slowly propagate outward during 13 hr of observations. Inside this region the Alfvénic Mach number is of the order of M A ≃ 0.02–0.11, the plasma β is close to unity, and the level of turbulence is higher than in the surrounding corona, but decreases slowly with time. All these results provide one of the most complete pictures of these features, and support the idea of a magnetic reconnection coupled with turbulence, thus allowing significant heating of the local plasma, despite the weakness of involved coronal magnetic fields in the considered altitude range.

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Space weather-related activities and projects on-going at INAF-Turin Observatory

Bemporad,

Fineschi,

Abbo

et al. 2023

Rend. Fis. Acc. Lincei

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The Solar Physics Group at the INAF-Turin Astrophysical Observatory (OATo) is actually involved in different Space Weather (SW) projects and missions. In particular, this Group is currently providing for the ESA SWESNET portal two new data analysis tools aimed at (1) the automated identification of magnetic flux ropes from the in situ data (CME magnetic effectiveness tool) and (2) the automated identification and arrival prediction of CMEs from remote sensing and in situ data (CME propagation and forecast tool). The Group is also developing numerical tools for future applications of interest for SW under the project SWELTO-Space WEather Laboratory in Turin Observatory. Moreover, the Group is participating in two SW missions, and in particular in Helianthus (research and development project on solar photonic propulsion for early SW warnings) and Selene (Solar Exploration by Lunar Eclipsing with Nanosatellites Experiment). In addition to this, the Group is leading or is involved in other “SW enabling science” projects, and in particular the Metis coronagraph on-board ESA Solar Orbiter mission, the ASPIICS coronagraph on-board ESA PROBA-3 mission, and the CorMag coronagraph on-board HEMERA stratospheric balloon. In this framework, the OATo Solar Physics Group is working on fundamental research on “SW enabling science”, dealing with the origin and acceleration of solar wind and Coronal Mass Ejections with remote-sensing data, and their interplanetary propagation and evolution with in situ data.

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Is There a Dynamic Difference between Stealthy and Standard Coronal Mass Ejections?

Cited by 3 publications

References 73 publications

Energetics of a Solar Flare and a Coronal Mass Ejection Generated by a Hot Channel Eruption

Energetics of a Solar Flare and a Coronal Mass Ejection Generated by a Hot Channel Eruption

First Determination in the Extended Corona of the 2D Thermal Evolution of a Current Sheet after a Solar Eruption

Space weather-related activities and projects on-going at INAF-Turin Observatory

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