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| Format: | Preprint |
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2025
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| Online Access: | https://arxiv.org/abs/2501.02753 |
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| _version_ | 1866915193664045056 |
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| author | Xue, Li Jiao, Cheng-Liang Zhang, Li-Xin |
| author_facet | Xue, Li Jiao, Cheng-Liang Zhang, Li-Xin |
| contents | We establish a spherically symmetric model of solar atmosphere, which consists of the whole chromosphere and low corona below the $1.25$ solar radius. It is a hydrodynamic model with heating in the chromosphere through an artificial energy flux. We performed a series of simulations with our model and found oscillations with a peak frequency of $\sim$4 $\rm{mHz}$ in the power spectrum. We confirmed that this resulted from the $p$-mode excited in the transition region and amplified in a resonant cavity situated in the height range $\sim$$4\times10^3$--$2\times10^4$ km. This result is consistent with global observations of Alfvénic waves in corona and can naturally explain the observational ubiquity of $4\ \rm{mHz}$ without the difficulty of the $p$-mode passing through the acoustic-damping chromosphere. We also confirmed that acoustic shock waves alone cannot heat the corona to the observed temperature, and found mass upflows in the height range $\sim$$7\times10^3$--$7\times10^4$ km in our model, which pumped the dense and cool plasma into the corona and might be the mass supplier for solar prominences. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2501_02753 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A Scenario for Origin of Global 4 mHz Oscillations in Solar Corona Xue, Li Jiao, Cheng-Liang Zhang, Li-Xin Solar and Stellar Astrophysics We establish a spherically symmetric model of solar atmosphere, which consists of the whole chromosphere and low corona below the $1.25$ solar radius. It is a hydrodynamic model with heating in the chromosphere through an artificial energy flux. We performed a series of simulations with our model and found oscillations with a peak frequency of $\sim$4 $\rm{mHz}$ in the power spectrum. We confirmed that this resulted from the $p$-mode excited in the transition region and amplified in a resonant cavity situated in the height range $\sim$$4\times10^3$--$2\times10^4$ km. This result is consistent with global observations of Alfvénic waves in corona and can naturally explain the observational ubiquity of $4\ \rm{mHz}$ without the difficulty of the $p$-mode passing through the acoustic-damping chromosphere. We also confirmed that acoustic shock waves alone cannot heat the corona to the observed temperature, and found mass upflows in the height range $\sim$$7\times10^3$--$7\times10^4$ km in our model, which pumped the dense and cool plasma into the corona and might be the mass supplier for solar prominences. |
| title | A Scenario for Origin of Global 4 mHz Oscillations in Solar Corona |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2501.02753 |