Magnetic, Kinetic, and Transition Regime: Spatially-Segregated Structure of Compressive MHD Turbulence
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arXiv
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| Format: | Preprint |
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2024
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| _version_ | 1866918121521020928 |
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| author | Li, Guang-Xing Zhao, Mengke |
| author_facet | Li, Guang-Xing Zhao, Mengke |
| contents | Turbulence is a complex physical process prevalent in modern physics, particularly in ionized environments like interstellar gas, where magnetic fields play a dynamic role. However, the precise influence of magnetic fields in such settings remains unclear. We employ the Alfvén Mach number, ${M}_{\mathrm{A}} = \sqrt{E_{\mathrm{k}}/E_{\mathrm{B}}}$, to gauge the magnetic field's significance relative to turbulent motion, uncovering diverse interaction patterns. In the low-${M}_{\mathrm{A}}$ magnetic regime, the field is force-free, yet gas motion does not align with it. At intermediate ${M}_{\mathrm{A}}$ (magnetic-kinetic transition regime), velocity and magnetic fields show peak alignment, likely due to rapid relaxation. In the high-${M}_{\mathrm{A}}$ kinetic regime, both fields are irregular and unaligned. These regimes find observational counterparts in interstellar gas, highlighting the multifaceted nature of MHD turbulence and aiding future astrophysical interpretations. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2409_02769 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Magnetic, Kinetic, and Transition Regime: Spatially-Segregated Structure of Compressive MHD Turbulence Li, Guang-Xing Zhao, Mengke Astrophysics of Galaxies Solar and Stellar Astrophysics Computational Physics Plasma Physics Turbulence is a complex physical process prevalent in modern physics, particularly in ionized environments like interstellar gas, where magnetic fields play a dynamic role. However, the precise influence of magnetic fields in such settings remains unclear. We employ the Alfvén Mach number, ${M}_{\mathrm{A}} = \sqrt{E_{\mathrm{k}}/E_{\mathrm{B}}}$, to gauge the magnetic field's significance relative to turbulent motion, uncovering diverse interaction patterns. In the low-${M}_{\mathrm{A}}$ magnetic regime, the field is force-free, yet gas motion does not align with it. At intermediate ${M}_{\mathrm{A}}$ (magnetic-kinetic transition regime), velocity and magnetic fields show peak alignment, likely due to rapid relaxation. In the high-${M}_{\mathrm{A}}$ kinetic regime, both fields are irregular and unaligned. These regimes find observational counterparts in interstellar gas, highlighting the multifaceted nature of MHD turbulence and aiding future astrophysical interpretations. |
| title | Magnetic, Kinetic, and Transition Regime: Spatially-Segregated Structure of Compressive MHD Turbulence |
| topic | Astrophysics of Galaxies Solar and Stellar Astrophysics Computational Physics Plasma Physics |
| url | https://arxiv.org/abs/2409.02769 |