Helmet streamer influence on the evolution of magnetic flux ropes
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| Main Authors: | , , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866918018026569728 |
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| author | Cécere, M. Wyper, P. F. Krause, G. Sahade, A. Rice, O. E. K. |
| author_facet | Cécere, M. Wyper, P. F. Krause, G. Sahade, A. Rice, O. E. K. |
| contents | Context: Solar eruptions are crucial for space weather studies. Understanding the mechanisms influencing their evolution is key to improving predictions of their geoeffectiveness. Helmet streamers (HSs) are persistent structures in the solar corona, present in both minimum and maximum solar activity periods. These structures contain a current sheet of low magnetic energy, where coronal mass ejections (CMEs) tend to deflect. However, they also feature a closed magnetic field region beneath this sheet, often confining eruptions. Their complexity makes predicting eruptions challenging. Aims: This study examines how HSs influence the evolution and potential confinement of magnetic flux ropes (MFRs). We explore magnetic configurations where the MFR is more likely to rise through the overlying field, aiming to establish simple parameters that help predict whether an MFR will ascend or remain confined. Methods: Using 2.5D MHD simulations, we model MFR dynamics in the presence of an HS, analyzing different magnetic configurations and focusing on the mechanisms that enable ascent or confinement. Results: Null-point reconnection plays a key role in MFR dynamics. Depending on the initial configuration, it can either disrupt the MFR, preventing ascent, or reduce the strapping flux, facilitating upward motion. We identify a critical threshold: if the strapping flux above the MFR is less than two-thirds of its poloidal flux, the MFR ascends successfully. Conclusions: Our simulations show that null-point reconnection significantly impacts MFR ascent. A key predictor of successful rise is the initial ratio of the MFR's poloidal flux to the strapping flux above it. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2503_19905 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Helmet streamer influence on the evolution of magnetic flux ropes Cécere, M. Wyper, P. F. Krause, G. Sahade, A. Rice, O. E. K. Solar and Stellar Astrophysics Plasma Physics Context: Solar eruptions are crucial for space weather studies. Understanding the mechanisms influencing their evolution is key to improving predictions of their geoeffectiveness. Helmet streamers (HSs) are persistent structures in the solar corona, present in both minimum and maximum solar activity periods. These structures contain a current sheet of low magnetic energy, where coronal mass ejections (CMEs) tend to deflect. However, they also feature a closed magnetic field region beneath this sheet, often confining eruptions. Their complexity makes predicting eruptions challenging. Aims: This study examines how HSs influence the evolution and potential confinement of magnetic flux ropes (MFRs). We explore magnetic configurations where the MFR is more likely to rise through the overlying field, aiming to establish simple parameters that help predict whether an MFR will ascend or remain confined. Methods: Using 2.5D MHD simulations, we model MFR dynamics in the presence of an HS, analyzing different magnetic configurations and focusing on the mechanisms that enable ascent or confinement. Results: Null-point reconnection plays a key role in MFR dynamics. Depending on the initial configuration, it can either disrupt the MFR, preventing ascent, or reduce the strapping flux, facilitating upward motion. We identify a critical threshold: if the strapping flux above the MFR is less than two-thirds of its poloidal flux, the MFR ascends successfully. Conclusions: Our simulations show that null-point reconnection significantly impacts MFR ascent. A key predictor of successful rise is the initial ratio of the MFR's poloidal flux to the strapping flux above it. |
| title | Helmet streamer influence on the evolution of magnetic flux ropes |
| topic | Solar and Stellar Astrophysics Plasma Physics |
| url | https://arxiv.org/abs/2503.19905 |