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Magnetic evolution of active regions: formation and eruption of magnetic flux ropes
Solar and Stellar Astrophysics · Submitted 3 Oct 2024
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Therefore, coronal helicity accumulation leads to twisted FR formation and its eruption.
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The abstract, sentence by sentence
Magnetic flux ropes (FRs) are twisted structures appearing on the sun, predominantly in the magnetically concentrated regions. These structures appear as coronal features known as filaments or prominences in H$\alpha$ observations, and as sigmoids in X-ray, EUV observations. Using the continuous vector magnetic field observations from \textit{Helioseismic and Magnetic Imager} onboard \textit{Solar Dynamics Observatory}, we study the evolution of the magnetic fields in the active regions (ARs) to understand the conditions of twisted flux formation. While ARs emerge and evolve further, flux motions such as shearing and rotation are efficient mechanisms to form twisted flux ropes. Magnetic helicity quantifies the twisted magnetic fields and helicity injection through photosphere leads to its accumulation in the corona. Therefore, coronal helicity accumulation leads to twisted FR formation and its eruption. The magnetic helicity injection is seen to evolve distinctly in the regions of flux rope formation and eruption. The ARs that are associated with eruptive activity are observed with helicity injection predominantly with one sign over a period of a few days. The ARs that inject helicity with a changing sign are unlikely to form twisted FRs because coronal helicity during the period of one sign of injected helicity gets cancelled by the opposite sign of injection in the later period. As a result, the coronal field reconfigures from shared to potential structure. For a given AR, the upper limit of helicity that could cause a CME eruption is not yet understood, which can be the subject of future studies of ARs. Magnetic reconnection plays a crucial role in both the initiation and driving of FR eruptions after their formation. Data-driven simulations of the AR evolution provide more insights on the flux rope formation and its onset of eruption.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Magnetic flux ropes (FRs) are twisted structures appearing on the sun, predominantly in the magnetically concentrated regions. | background 1.00 | 0.05 | 0.02 | asserted 1.00 |
| s1 | These structures appear as coronal features known as filaments or prominences in H$\alpha$ observations, and as sigmoids in X-ray, EUV observations. | background 1.00 | 0.07 | 0.02 | asserted 1.00 |
| s2 | Using the continuous vector magnetic field observations from \textit{Helioseismic and Magnetic Imager} onboard \textit{Solar Dynamics Observatory}, we study the evolution of the magnetic fields in the active regions (ARs) to understand the conditions of twisted flux formation. | method 0.61 | 0.94 | 0.03 | asserted 0.92 |
| s3 | While ARs emerge and evolve further, flux motions such as shearing and rotation are efficient mechanisms to form twisted flux ropes. | background 0.98 | 0.13 | 0.05 | asserted 0.96 |
| s4 | Magnetic helicity quantifies the twisted magnetic fields and helicity injection through photosphere leads to its accumulation in the corona. | background 1.00 | 0.07 | 0.04 | asserted 1.00 |
| s5 | Therefore, coronal helicity accumulation leads to twisted FR formation and its eruption. | interpretation 0.67 | 0.15 | 0.51 | asserted 1.00 |
| s6 | The magnetic helicity injection is seen to evolve distinctly in the regions of flux rope formation and eruption. | result 0.98 | 0.79 | 0.11 | asserted 1.00 |
| s7 | The ARs that are associated with eruptive activity are observed with helicity injection predominantly with one sign over a period of a few days. | result 1.00 | 0.79 | 0.18 | asserted 1.00 |
| s8 | The ARs that inject helicity with a changing sign are unlikely to form twisted FRs because coronal helicity during the period of one sign of injected helicity gets cancelled by the opposite sign of injection in the later period. | interpretation 0.62 | 0.47 | 0.18 | hedged possibility 0.65 |
| s9 | As a result, the coronal field reconfigures from shared to potential structure. | interpretation 0.74 | 0.30 | 0.07 | asserted 1.00 |
| s10 | For a given AR, the upper limit of helicity that could cause a CME eruption is not yet understood, which can be the subject of future studies of ARs. | future work 0.80 | 0.06 | 0.04 | asserted 0.55 |
| s11 | Magnetic reconnection plays a crucial role in both the initiation and driving of FR eruptions after their formation. | background 0.91 | 0.12 | 0.08 | asserted 1.00 |
| s12 | Data-driven simulations of the AR evolution provide more insights on the flux rope formation and its onset of eruption. | method 0.58 | 0.27 | 0.05 | asserted 0.85 |
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Original abstract
Magnetic flux ropes (FRs) are twisted structures appearing on the sun, predominantly in the magnetically concentrated regions. These structures appear as coronal features known as filaments or prominences in H$\alpha$ observations, and as sigmoids in X-ray, EUV observations. Using the continuous vector magnetic field observations from \textit{Helioseismic and Magnetic Imager} onboard \textit{Solar Dynamics Observatory}, we study the evolution of the magnetic fields in the active regions (ARs) to understand the conditions of twisted flux formation. While ARs emerge and evolve further, flux motions such as shearing and rotation are efficient mechanisms to form twisted flux ropes. Magnetic helicity quantifies the twisted magnetic fields and helicity injection through photosphere leads to its accumulation in the corona. Therefore, coronal helicity accumulation leads to twisted FR formation and its eruption. The magnetic helicity injection is seen to evolve distinctly in the regions of flux rope formation and eruption. The ARs that are associated with eruptive activity are observed with helicity injection predominantly with one sign over a period of a few days. The ARs that inject helicity with a changing sign are unlikely to form twisted FRs because coronal helicity during the period of one sign of injected helicity gets cancelled by the opposite sign of injection in the later period. As a result, the coronal field reconfigures from shared to potential structure. For a given AR, the upper limit of helicity that could cause a CME eruption is not yet understood, which can be the subject of future studies of ARs. Magnetic reconnection plays a crucial role in both the initiation and driving of FR eruptions after their formation. Data-driven simulations of the AR evolution provide more insights on the flux rope formation and its onset of eruption.
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