A self-consistent numerical model of internal wave-induced mean flow oscillations in polar geometry
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arXiv
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| Format: | Preprint |
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2025
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| _version_ | 1866918331292844032 |
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| author | Daniel, Florentin Lecoanet, Daniel |
| author_facet | Daniel, Florentin Lecoanet, Daniel |
| contents | The Earth's Quasi-Biennial Oscillation (QBO) is a natural example of wave-mean flow interaction and corresponds to the alternating directions of winds in the equatorial stratosphere. It is due to internal gravity waves (IGW) generated in the underlying convective troposphere. In stars, a similar situation is predicted to occur, with the interaction of a stably-stratified radiative zone and a convective zone. In this context, we investigate the dynamics of this reversing mean flow by modelling a stably-stratified envelope and a convectively unstable core in polar geometry. Here, the coupling between the two zones is achieved self-consistently, and IGW generated through convection lead to the formation of a reversing azimuthal mean flow in the upper layer. We characterise the mean-flow oscillations by their periods, velocity amplitudes, and regularity. Despite a continuous broad spectrum of IGW, our work show good qualitative agreement with the monochromatic model of Plumb and McEwan (1978). If the latter was originally developed in the context of the Earth's QBO, our study could prove relevant for its stellar counterpart in massive stars, which host convective cores and radiative envelopes. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2509_19482 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A self-consistent numerical model of internal wave-induced mean flow oscillations in polar geometry Daniel, Florentin Lecoanet, Daniel Solar and Stellar Astrophysics Fluid Dynamics The Earth's Quasi-Biennial Oscillation (QBO) is a natural example of wave-mean flow interaction and corresponds to the alternating directions of winds in the equatorial stratosphere. It is due to internal gravity waves (IGW) generated in the underlying convective troposphere. In stars, a similar situation is predicted to occur, with the interaction of a stably-stratified radiative zone and a convective zone. In this context, we investigate the dynamics of this reversing mean flow by modelling a stably-stratified envelope and a convectively unstable core in polar geometry. Here, the coupling between the two zones is achieved self-consistently, and IGW generated through convection lead to the formation of a reversing azimuthal mean flow in the upper layer. We characterise the mean-flow oscillations by their periods, velocity amplitudes, and regularity. Despite a continuous broad spectrum of IGW, our work show good qualitative agreement with the monochromatic model of Plumb and McEwan (1978). If the latter was originally developed in the context of the Earth's QBO, our study could prove relevant for its stellar counterpart in massive stars, which host convective cores and radiative envelopes. |
| title | A self-consistent numerical model of internal wave-induced mean flow oscillations in polar geometry |
| topic | Solar and Stellar Astrophysics Fluid Dynamics |
| url | https://arxiv.org/abs/2509.19482 |