Neutron Star Atmosphere-Ocean Dynamics
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arXiv
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| Autores principales: | , , , , |
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| Formato: | Preprint |
| Publicado: |
2023
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| _version_ | 1866917684666433536 |
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| author | Nättilä, Joonas Cho, James Y-K. Skinner, Jack W. Most, Elias R. Ripperda, Bart |
| author_facet | Nättilä, Joonas Cho, James Y-K. Skinner, Jack W. Most, Elias R. Ripperda, Bart |
| contents | We analyze the structure and dynamics of the plasma atmospheres and Coulomb-liquid oceans on neutron stars. Salient dynamical parameters are identified and their values estimated for the governing set of magnetohydrodynamics equations. Neutron star atmospheres and oceans are strongly stratified and, depending on the rotation period, contain a multitude of long-lived vortices (spots) and/or narrow zonal jets (free-shear zones) in the large plasma-beta regime - i.e., $β_p \gg 1$ (hydrodynamic regime). In contrast, when $β_p \lesssim 1$ (magnetohydrodynamic regime), the flow is dominated by a global lattice of effectively fixed magnetic islands (plasmoids) - without any jets. Understanding the spatio-temporal variability of dynamic atmospheres and oceans on neutron stars is crucial for interpreting observations of their X-ray emissions. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2306_08186 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Neutron Star Atmosphere-Ocean Dynamics Nättilä, Joonas Cho, James Y-K. Skinner, Jack W. Most, Elias R. Ripperda, Bart High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We analyze the structure and dynamics of the plasma atmospheres and Coulomb-liquid oceans on neutron stars. Salient dynamical parameters are identified and their values estimated for the governing set of magnetohydrodynamics equations. Neutron star atmospheres and oceans are strongly stratified and, depending on the rotation period, contain a multitude of long-lived vortices (spots) and/or narrow zonal jets (free-shear zones) in the large plasma-beta regime - i.e., $β_p \gg 1$ (hydrodynamic regime). In contrast, when $β_p \lesssim 1$ (magnetohydrodynamic regime), the flow is dominated by a global lattice of effectively fixed magnetic islands (plasmoids) - without any jets. Understanding the spatio-temporal variability of dynamic atmospheres and oceans on neutron stars is crucial for interpreting observations of their X-ray emissions. |
| title | Neutron Star Atmosphere-Ocean Dynamics |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2306.08186 |