Observations of microwave emission from solar jets and comparison with MHD simulations
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arXiv
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| Autores principales: | , , |
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| Formato: | Preprint |
| Publicado: |
2025
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| Acceso en línea: | |
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| _version_ | 1866913952704757760 |
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| author | Alissandrakis, Costas E. Archontis, Vasilis Moraitis, Kostas |
| author_facet | Alissandrakis, Costas E. Archontis, Vasilis Moraitis, Kostas |
| contents | We computed the thermal microwave emission from a 3D magnetohydrodynamic (MHD) simulation and compared it with observations of solar jets. The simulation treats the emergence of magnetic flux into the solar atmosphere and its interaction with a low, pre-existing ambient magnetic field. This interaction leads to the formation and development of a jet, driven by an eruption. The computed 17 GHz radio emission is compared with a number of observed jets, with respect to their morphology, their flux, and the rise time of the radio flux. We find that the MHD model reproduces the characteristics of lower-intensity jets reasonably well, whereas there are differences with stronger jets. We suggest possible ways to obtain more realistic jets from MHD simulations, so that they match better the real jets. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_16234 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Observations of microwave emission from solar jets and comparison with MHD simulations Alissandrakis, Costas E. Archontis, Vasilis Moraitis, Kostas Solar and Stellar Astrophysics We computed the thermal microwave emission from a 3D magnetohydrodynamic (MHD) simulation and compared it with observations of solar jets. The simulation treats the emergence of magnetic flux into the solar atmosphere and its interaction with a low, pre-existing ambient magnetic field. This interaction leads to the formation and development of a jet, driven by an eruption. The computed 17 GHz radio emission is compared with a number of observed jets, with respect to their morphology, their flux, and the rise time of the radio flux. We find that the MHD model reproduces the characteristics of lower-intensity jets reasonably well, whereas there are differences with stronger jets. We suggest possible ways to obtain more realistic jets from MHD simulations, so that they match better the real jets. |
| title | Observations of microwave emission from solar jets and comparison with MHD simulations |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2507.16234 |