The magnetohydrodynamic equations in terms of waveframe variables
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arXiv
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| Hauptverfasser: | , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866911758461960192 |
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| author | Van Doorsselaere, Tom Magyar, Norbert Sieyra, M. Valeria Goossens, Marcel |
| author_facet | Van Doorsselaere, Tom Magyar, Norbert Sieyra, M. Valeria Goossens, Marcel |
| contents | Generalising the Elsasser variables, we introduce the Q-variables. These are more flexible than the Elsasser variables, because they also allow to track waves with phase speeds different than the Alfven speed. We rewrite the MHD equations with these Q-variables. We consider also the linearised version of the resulting MHD equations in a uniform plasma, and recover the classical Alfven waves, but also separate the fast and slow magnetosonic waves in upward and downward propagating waves. Moreover, we show that the Q-variables may also track the upward and downward propagating surface Alfven waves in a non-uniform plasma, displaying the power of our generalisation. In the end, we lay the mathematical framework for driving solar wind models with a multitude of wave drivers. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2401_07830 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The magnetohydrodynamic equations in terms of waveframe variables Van Doorsselaere, Tom Magyar, Norbert Sieyra, M. Valeria Goossens, Marcel Plasma Physics Solar and Stellar Astrophysics Generalising the Elsasser variables, we introduce the Q-variables. These are more flexible than the Elsasser variables, because they also allow to track waves with phase speeds different than the Alfven speed. We rewrite the MHD equations with these Q-variables. We consider also the linearised version of the resulting MHD equations in a uniform plasma, and recover the classical Alfven waves, but also separate the fast and slow magnetosonic waves in upward and downward propagating waves. Moreover, we show that the Q-variables may also track the upward and downward propagating surface Alfven waves in a non-uniform plasma, displaying the power of our generalisation. In the end, we lay the mathematical framework for driving solar wind models with a multitude of wave drivers. |
| title | The magnetohydrodynamic equations in terms of waveframe variables |
| topic | Plasma Physics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2401.07830 |