The Interaction between Solar Convection and Rotation
Fuente:
arXiv
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| Autores principales: | , |
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| Formato: | Preprint |
| Publicado: |
2024
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| Materias: | |
| Acceso en línea: | |
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| _version_ | 1866913199590211584 |
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| author | Chen, Haibin Wu, Rong |
| author_facet | Chen, Haibin Wu, Rong |
| contents | The rotational energy of a fluid parcel changes during isotropic expansion or compression. In solar convection, rotation absorbs energy from convection and inhibits it, causing the motion of fluid parcels larger than a critical size to become vibration. Turbulence and inertial oscillations can cause the deformation of fluid parcels to deviate from isotropic, altering the equilibrium position of the vibration and forming motion larger than the critical size, respectively, the large granules within the granules and probably the mesogranulation. The change in rotational energy of granules during convection causes their rotation speed to differ from the local speed, forming a statistically significant solar radial differential rotation. The meridional circulation driven by radial differential rotation transports angular momentum towards the equator, forming the latitudinal differential rotation. A model constructed by combining mixing length theory explains why granule size and temperature distribution are independent of latitude, and the structure produced by this mechanism is similar to the characteristics of supergranules. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2401_10105 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The Interaction between Solar Convection and Rotation Chen, Haibin Wu, Rong Solar and Stellar Astrophysics Fluid Dynamics The rotational energy of a fluid parcel changes during isotropic expansion or compression. In solar convection, rotation absorbs energy from convection and inhibits it, causing the motion of fluid parcels larger than a critical size to become vibration. Turbulence and inertial oscillations can cause the deformation of fluid parcels to deviate from isotropic, altering the equilibrium position of the vibration and forming motion larger than the critical size, respectively, the large granules within the granules and probably the mesogranulation. The change in rotational energy of granules during convection causes their rotation speed to differ from the local speed, forming a statistically significant solar radial differential rotation. The meridional circulation driven by radial differential rotation transports angular momentum towards the equator, forming the latitudinal differential rotation. A model constructed by combining mixing length theory explains why granule size and temperature distribution are independent of latitude, and the structure produced by this mechanism is similar to the characteristics of supergranules. |
| title | The Interaction between Solar Convection and Rotation |
| topic | Solar and Stellar Astrophysics Fluid Dynamics |
| url | https://arxiv.org/abs/2401.10105 |