Radiative hydrodynamic simulations of FIP fractionation in solar flares
Fuente:
arXiv
Enregistré dans:
| Auteurs principaux: | , , , , , , , |
|---|---|
| Format: | Preprint |
| Publié: |
2025
|
| Sujets: | |
| Accès en ligne: | |
| Tags: |
Ajouter un tag
Pas de tags, Soyez le premier à ajouter un tag!
|
| _version_ | 1866912742097551360 |
|---|---|
| author | Reep, Jeffrey W. Benavitz, Luke Fushimi To, Andy S. H. Brooks, David H. Laming, J. Martin Antolin, Patrick Long, David M. Baker, Deborah |
| author_facet | Reep, Jeffrey W. Benavitz, Luke Fushimi To, Andy S. H. Brooks, David H. Laming, J. Martin Antolin, Patrick Long, David M. Baker, Deborah |
| contents | Elemental abundances in solar flares are observed to vary both spatially and temporally, but the underlying mechanisms remain poorly understood. There is an interplay between advection and the preferential acceleration of low first ionization potential (FIP) elements that likely shapes the observed abundance distributions. Models of the FIP effect predict enhancements near loop footpoints that diffuse upward over time. We simulate strong evaporation events that advect this low-FIP enhancement into the corona. When the enhancement is sharply peaked, the corona does not become fractionated, exhibiting only a localized abundance peak near the loop apex that facilitates coronal rain formation. In contrast, a broad enhancement with relatively weak heating yields a uniformly fractionated corona, which is not sufficient for coronal rain formation. As the heating rate increases, the low-FIP enhanced plasma is increasingly compressed toward the loop apex, and rain is able to form. These results suggest a potential observational correlation between the presence and amount of coronal rain, the strength of flare heating, and the fractionation process itself. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2509_25695 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Radiative hydrodynamic simulations of FIP fractionation in solar flares Reep, Jeffrey W. Benavitz, Luke Fushimi To, Andy S. H. Brooks, David H. Laming, J. Martin Antolin, Patrick Long, David M. Baker, Deborah Solar and Stellar Astrophysics Elemental abundances in solar flares are observed to vary both spatially and temporally, but the underlying mechanisms remain poorly understood. There is an interplay between advection and the preferential acceleration of low first ionization potential (FIP) elements that likely shapes the observed abundance distributions. Models of the FIP effect predict enhancements near loop footpoints that diffuse upward over time. We simulate strong evaporation events that advect this low-FIP enhancement into the corona. When the enhancement is sharply peaked, the corona does not become fractionated, exhibiting only a localized abundance peak near the loop apex that facilitates coronal rain formation. In contrast, a broad enhancement with relatively weak heating yields a uniformly fractionated corona, which is not sufficient for coronal rain formation. As the heating rate increases, the low-FIP enhanced plasma is increasingly compressed toward the loop apex, and rain is able to form. These results suggest a potential observational correlation between the presence and amount of coronal rain, the strength of flare heating, and the fractionation process itself. |
| title | Radiative hydrodynamic simulations of FIP fractionation in solar flares |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2509.25695 |