Revisiting turbulent properties of solar convection with 3D radiative hydrodynamic modeling
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arXiv
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| Auteurs principaux: | , |
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| Format: | Preprint |
| Publié: |
2025
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| _version_ | 1866909473088471040 |
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| author | Kitiashvili, Irina N. Wray, Alan A. |
| author_facet | Kitiashvili, Irina N. Wray, Alan A. |
| contents | We discuss the turbulent structure and dynamics of the upper solar convection zone using a 3D radiative hydrodynamic simulation model at 45 degrees latitude. The model reveals the self-formation of meridional flows, the leptocline, and the radial differential rotation. Unlike previous studies, the model shows a complex variation of the characteristic scales of turbulent flows with depth. In particular, an increase in the characteristic convective scale is trackable within an individual snapshot up to a depth of 7 Mm, near the bottom of the hydrogen ionization zone, where turbulent flows become weaker and more homogeneous. However, the turbulent spectra show an increase in scale with depth and a qualitative change in convective patterns below 7 Mm (near the bottom of the leptocline), suggesting changes in the diffusivity properties and energy exchange among different scales. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2502_00974 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Revisiting turbulent properties of solar convection with 3D radiative hydrodynamic modeling Kitiashvili, Irina N. Wray, Alan A. Solar and Stellar Astrophysics Space Physics We discuss the turbulent structure and dynamics of the upper solar convection zone using a 3D radiative hydrodynamic simulation model at 45 degrees latitude. The model reveals the self-formation of meridional flows, the leptocline, and the radial differential rotation. Unlike previous studies, the model shows a complex variation of the characteristic scales of turbulent flows with depth. In particular, an increase in the characteristic convective scale is trackable within an individual snapshot up to a depth of 7 Mm, near the bottom of the hydrogen ionization zone, where turbulent flows become weaker and more homogeneous. However, the turbulent spectra show an increase in scale with depth and a qualitative change in convective patterns below 7 Mm (near the bottom of the leptocline), suggesting changes in the diffusivity properties and energy exchange among different scales. |
| title | Revisiting turbulent properties of solar convection with 3D radiative hydrodynamic modeling |
| topic | Solar and Stellar Astrophysics Space Physics |
| url | https://arxiv.org/abs/2502.00974 |