The Sun's differential rotation is controlled by high-latitude baroclinically unstable inertial modes
Fuente:
arXiv
Saved in:
| Main Authors: | , , |
|---|---|
| Format: | Preprint |
| Published: |
2024
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866910388308672512 |
|---|---|
| author | Bekki, Yuto Cameron, Robert H. Gizon, Laurent |
| author_facet | Bekki, Yuto Cameron, Robert H. Gizon, Laurent |
| contents | Rapidly rotating fluids have a rotation profile which depends only on the distance from the rotation axis, in accordance with the Taylor-Proudman theorem. Although the Sun was expected to be such a body, helioseismology showed that the rotation rate in the convection zone is closer to constant on radii. It has been postulated that this deviation is due to the poles being warmer than the equator by a few degrees. Using numerical simulations, we show that the pole-to-equator temperature difference cannot exceed 7 Kelvin as a result of the back-reaction of the high-latitude baroclinically unstable inertial modes. The observed amplitudes of the modes further indicate that this maximum temperature difference is reached in the Sun. We conclude that the Sun's latitudinal differential rotation reaches its maximum allowed value. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2403_18986 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The Sun's differential rotation is controlled by high-latitude baroclinically unstable inertial modes Bekki, Yuto Cameron, Robert H. Gizon, Laurent Solar and Stellar Astrophysics Fluid Dynamics Rapidly rotating fluids have a rotation profile which depends only on the distance from the rotation axis, in accordance with the Taylor-Proudman theorem. Although the Sun was expected to be such a body, helioseismology showed that the rotation rate in the convection zone is closer to constant on radii. It has been postulated that this deviation is due to the poles being warmer than the equator by a few degrees. Using numerical simulations, we show that the pole-to-equator temperature difference cannot exceed 7 Kelvin as a result of the back-reaction of the high-latitude baroclinically unstable inertial modes. The observed amplitudes of the modes further indicate that this maximum temperature difference is reached in the Sun. We conclude that the Sun's latitudinal differential rotation reaches its maximum allowed value. |
| title | The Sun's differential rotation is controlled by high-latitude baroclinically unstable inertial modes |
| topic | Solar and Stellar Astrophysics Fluid Dynamics |
| url | https://arxiv.org/abs/2403.18986 |