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Helical flows along coronal loops following the launch of a coronal mass ejection
Solar and Stellar Astrophysics · Submitted 25 Feb 2025
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Following the launch of a CME, we find clear evidence for impulsive heating and expansion of plasma that travels a helical trajectory along a set of post-eruption loops.
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The abstract, sentence by sentence
Solar flares and coronal mass ejections (CMEs) are manifestations of energy release in the solar atmosphere, which can be accompanied by dynamic mass motions and waves in the surrounding atmosphere. Here, we present observations of plasma moving in a helical trajectory along a set of coronal loops formed following the eruption of a CME on 2024 May 14. This helical motion was observed in extreme ultraviolet (EUV) images from the Solar Dynamic Observatory (SDO), which provides new insights into plasma properties in a set of post-eruption coronal loops. We utilize images from the SDO Atmospheric Imaging Assembly (AIA) instrument to track the helical motion of plasma and to characterize its speed, acceleration, and physical properties. Additionally, we explore the evolution of the plasma density and temperature along the helical structure using the differential emission measure technique. The helical structure was visible in AIA for approximately 22 minutes, having a diameter of 22 Mm, and a total trajectory of nearly 184 Mm. Analysis of the AIA observations reveals that the plasma flow along this helical coronal loop exhibits speeds of 77-384 km s$^{-1}$ and temperatures ranging from 3.46 to 10.2 MK. Additionally, the densities were estimated to be between 4.3.106 and 1.55.107 cm-3, with an estimated magnetic field strength of 0.05-0.3 G. Following the launch of a CME, we find clear evidence for impulsive heating and expansion of plasma that travels a helical trajectory along a set of post-eruption loops. These observations provide an insight into impulsive plasma flows along coronal loops and indeed the topology of coronal loops.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Solar flares and coronal mass ejections (CMEs) are manifestations of energy release in the solar atmosphere, which can be accompanied by dynamic mass motions and waves in the surrounding atmosphere. | background 1.00 | 0.05 | 0.03 | hedged possibility 0.53 |
| s1 | Here, we present observations of plasma moving in a helical trajectory along a set of coronal loops formed following the eruption of a CME on 2024 May 14. | contribution 0.85 | 0.94 | 0.20 | asserted 1.00 |
| s2 | This helical motion was observed in extreme ultraviolet (EUV) images from the Solar Dynamic Observatory (SDO), which provides new insights into plasma properties in a set of post-eruption coronal loops. | contribution 0.39 | 0.74 | 0.11 | asserted 0.96 |
| s3 | We utilize images from the SDO Atmospheric Imaging Assembly (AIA) instrument to track the helical motion of plasma and to characterize its speed, acceleration, and physical properties. | method 0.99 | 0.96 | 0.03 | asserted 0.97 |
| s4 | Additionally, we explore the evolution of the plasma density and temperature along the helical structure using the differential emission measure technique. | method 0.95 | 0.95 | 0.03 | asserted 0.83 |
| s5 | The helical structure was visible in AIA for approximately 22 minutes, having a diameter of 22 Mm, and a total trajectory of nearly 184 Mm. | result 1.00 | 0.91 | 0.04 | asserted 1.00 |
| s6 | Analysis of the AIA observations reveals that the plasma flow along this helical coronal loop exhibits speeds of 77-384 km s$^{-1}$ and temperatures ranging from 3.46 to 10.2 MK. | result 1.00 | 0.95 | 0.11 | asserted 1.00 |
| s7 | Additionally, the densities were estimated to be between 4.3.106 and 1.55.107 cm-3, with an estimated magnetic field strength of 0.05-0.3 G. | result 1.00 | 0.93 | 0.05 | asserted 0.93 |
| s8 | Following the launch of a CME, we find clear evidence for impulsive heating and expansion of plasma that travels a helical trajectory along a set of post-eruption loops. | result 0.99 | 0.96 | 0.81 | asserted 1.00 |
| s9 | These observations provide an insight into impulsive plasma flows along coronal loops and indeed the topology of coronal loops. | interpretation 0.99 | 0.77 | 0.26 | asserted 0.69 |
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The paper
Original abstract
Solar flares and coronal mass ejections (CMEs) are manifestations of energy release in the solar atmosphere, which can be accompanied by dynamic mass motions and waves in the surrounding atmosphere. Here, we present observations of plasma moving in a helical trajectory along a set of coronal loops formed following the eruption of a CME on 2024 May 14. This helical motion was observed in extreme ultraviolet (EUV) images from the Solar Dynamic Observatory (SDO), which provides new insights into plasma properties in a set of post-eruption coronal loops. We utilize images from the SDO Atmospheric Imaging Assembly (AIA) instrument to track the helical motion of plasma and to characterize its speed, acceleration, and physical properties. Additionally, we explore the evolution of the plasma density and temperature along the helical structure using the differential emission measure technique. The helical structure was visible in AIA for approximately 22 minutes, having a diameter of 22 Mm, and a total trajectory of nearly 184 Mm. Analysis of the AIA observations reveals that the plasma flow along this helical coronal loop exhibits speeds of 77-384 km s$^{-1}$ and temperatures ranging from 3.46 to 10.2 MK. Additionally, the densities were estimated to be between 4.3.106 and 1.55.107 cm-3, with an estimated magnetic field strength of 0.05-0.3 G. Following the launch of a CME, we find clear evidence for impulsive heating and expansion of plasma that travels a helical trajectory along a set of post-eruption loops. These observations provide an insight into impulsive plasma flows along coronal loops and indeed the topology of coronal loops.
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