Strengthening of the f mode due to subsurface magnetic fields in simulations of convection
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arXiv
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| Format: | Preprint |
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2024
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| _version_ | 1866912041095135232 |
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| author | Kishore, G. Singh, Nishant K Käpylä, Petri Roth, Markus |
| author_facet | Kishore, G. Singh, Nishant K Käpylä, Petri Roth, Markus |
| contents | Previous studies have found that localized strengthening of the f mode recedes the emergence of active regions on the Sun by one day to three days. To help interpret these observations, we have performed nonlinear simulations of convection with imposed magnetic fields at different depths. We find that the f mode is strengthened when a super-equipartition magnetic field is imposed near the top of the domain. However, neither a magnetic field of equal strength near the bottom of the domain nor an equipartition magnetic field near the top of the domain have a significant effect. Our results suggest that the magnetic precursors of active regions are present near the surface of the Sun for much longer than would be expected if active regions were formed by flux tubes rising from deep within the convection zone. Application to observations should account for the fact that the effects we observe are transient. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2409_14840 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Strengthening of the f mode due to subsurface magnetic fields in simulations of convection Kishore, G. Singh, Nishant K Käpylä, Petri Roth, Markus Solar and Stellar Astrophysics Previous studies have found that localized strengthening of the f mode recedes the emergence of active regions on the Sun by one day to three days. To help interpret these observations, we have performed nonlinear simulations of convection with imposed magnetic fields at different depths. We find that the f mode is strengthened when a super-equipartition magnetic field is imposed near the top of the domain. However, neither a magnetic field of equal strength near the bottom of the domain nor an equipartition magnetic field near the top of the domain have a significant effect. Our results suggest that the magnetic precursors of active regions are present near the surface of the Sun for much longer than would be expected if active regions were formed by flux tubes rising from deep within the convection zone. Application to observations should account for the fact that the effects we observe are transient. |
| title | Strengthening of the f mode due to subsurface magnetic fields in simulations of convection |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2409.14840 |