Effect of Magnetic diffusion in the Chromosphere on the Solar Wind
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arXiv
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| Autori principali: | , , , |
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| Natura: | Preprint |
| Pubblicazione: |
2024
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| _version_ | 1866913344566329344 |
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| author | Matsuoka, Masato Suzuki, Takeru K. Tokuno, Takato Kakiuchi, Kensuke |
| author_facet | Matsuoka, Masato Suzuki, Takeru K. Tokuno, Takato Kakiuchi, Kensuke |
| contents | We investigate non-ideal magnetohydrodynamical (MHD) effects in the chromosphere on the solar wind by performing MHD simulations for Alfvén-wave driven winds with explicitly including Ohmic and ambipolar diffusion. We find that MHD waves are significantly damped in the chromosphere by ambipolar diffusion so that the Alfvénic Poynting flux that reaches the corona is substantially reduced. As a result, the coronal temperature and the mass loss rate of the solar wind are considerably reduced, compared with those obtained from an ideal MHD case, which is indicative of a great importance of the non-ideal MHD effects in the solar atmosphere. However, the temperature and the mass loss rate are recovered by a small increase in the convection-originated velocity perturbation at the photosphere because of the sensitive dependence of the ambipolar diffusion and reflection of Alfvén waves on the physical properties of the chromosphere. We also find that density perturbations in the corona are reduced by the ambipolar diffusion of Alfvén waves in the chromosphere because the nonlinear generation of compressible perturbations is suppressed. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2403_18409 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Effect of Magnetic diffusion in the Chromosphere on the Solar Wind Matsuoka, Masato Suzuki, Takeru K. Tokuno, Takato Kakiuchi, Kensuke Solar and Stellar Astrophysics We investigate non-ideal magnetohydrodynamical (MHD) effects in the chromosphere on the solar wind by performing MHD simulations for Alfvén-wave driven winds with explicitly including Ohmic and ambipolar diffusion. We find that MHD waves are significantly damped in the chromosphere by ambipolar diffusion so that the Alfvénic Poynting flux that reaches the corona is substantially reduced. As a result, the coronal temperature and the mass loss rate of the solar wind are considerably reduced, compared with those obtained from an ideal MHD case, which is indicative of a great importance of the non-ideal MHD effects in the solar atmosphere. However, the temperature and the mass loss rate are recovered by a small increase in the convection-originated velocity perturbation at the photosphere because of the sensitive dependence of the ambipolar diffusion and reflection of Alfvén waves on the physical properties of the chromosphere. We also find that density perturbations in the corona are reduced by the ambipolar diffusion of Alfvén waves in the chromosphere because the nonlinear generation of compressible perturbations is suppressed. |
| title | Effect of Magnetic diffusion in the Chromosphere on the Solar Wind |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2403.18409 |