Polarity inversion line helicities and solar eruptivity
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arXiv
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| Natura: | Preprint |
| Pubblicazione: |
2025
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| _version_ | 1866914053878710272 |
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| author | Moraitis, K. Thalmann, J. K. |
| author_facet | Moraitis, K. Thalmann, J. K. |
| contents | This work examines the relationship between solar eruptivity and the relative helicity that is contained around the polarity inversion line (PIL) of the magnetic field, along with its current-carrying component. To this end, we analyze the evolution of the PIL helicities in a sample of $\sim 40$ solar active regions which exhibited more than 200 flares of class M or higher. The computation of the PIL helicities is accomplished with the help of relative field line helicity, the recently-developed proxy for the density of relative helicity, following the extrapolation of the 3D coronal magnetic field with a nonlinear force-free method. We find that, on average, the relative helicity of the PIL decreases significantly, by more than $10\%$, during stronger eruptive flares (M5.0 class and above), while smaller changes are observed for confined and/or weaker flares. The PIL current-carrying helicity shows higher-magnitude decreases in both strong and weak flares, reaching $20\%$ average changes during the stronger eruptive flares. Notably, the PIL current-carrying helicity displays the most pronounced distinction between eruptive and confined flares, indicating its strong potential as a diagnostic of solar eruptivity. We discuss the implications of these findings for solar flare forecasting. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2509_19864 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Polarity inversion line helicities and solar eruptivity Moraitis, K. Thalmann, J. K. Solar and Stellar Astrophysics This work examines the relationship between solar eruptivity and the relative helicity that is contained around the polarity inversion line (PIL) of the magnetic field, along with its current-carrying component. To this end, we analyze the evolution of the PIL helicities in a sample of $\sim 40$ solar active regions which exhibited more than 200 flares of class M or higher. The computation of the PIL helicities is accomplished with the help of relative field line helicity, the recently-developed proxy for the density of relative helicity, following the extrapolation of the 3D coronal magnetic field with a nonlinear force-free method. We find that, on average, the relative helicity of the PIL decreases significantly, by more than $10\%$, during stronger eruptive flares (M5.0 class and above), while smaller changes are observed for confined and/or weaker flares. The PIL current-carrying helicity shows higher-magnitude decreases in both strong and weak flares, reaching $20\%$ average changes during the stronger eruptive flares. Notably, the PIL current-carrying helicity displays the most pronounced distinction between eruptive and confined flares, indicating its strong potential as a diagnostic of solar eruptivity. We discuss the implications of these findings for solar flare forecasting. |
| title | Polarity inversion line helicities and solar eruptivity |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2509.19864 |