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| Format: | Preprint |
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2025
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| Online Access: | https://arxiv.org/abs/2503.12135 |
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| _version_ | 1866917958410829824 |
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| author | Xie, Wei Lei, Wei-Hua |
| author_facet | Xie, Wei Lei, Wei-Hua |
| contents | Outflows/jets are ubiquitous in a wide range of astrophysical objects, yet the mechanisms responsible for their generation remain elusive. One hypothesis is that they are magnetically driven. Based on general relativistic MHD equations, we establish a formulation to describe the outflows driven by large-scale magnetic fields from the accretion disk in Schwarzschild spacetime. The outflow solution manifests as a contour level of a ``Bernoulli" function, which is determined by ensuring that it passes through both the slow and fast magnetosonic points. This approach is a general relativistic extension to the classical treatment of Cao and Spruit (1994). The initial plasma $β$ that permits magnetically driven outflow solutions is constrained, with the slow magnetosonic point above the footpoint setting an upper limit ($β_\mathrm{b}\lesssim 2$) and the Alfvén point inside the light cylinder setting a lower limit ($β_\mathrm{b}\gtrsim 0.02$). The higher the magnetization, the higher the temperature allowed, leading to relativistic outflows/jets. We investigate the relativistic outflows/jets of several typical objects such as active galactic nuclei (AGN), X-ray binaries (XRBs) and gamma-ray bursts (GRBs). The results indicate that all of these phenomena require strongly magnetized, high-temperature outflows as initial conditions, suggesting a potential association between the production of relativistic outflows/jets and corona-like structures. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_12135 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The relativistic outflow driven by the large-scale magnetic field from an accretion disk Xie, Wei Lei, Wei-Hua High Energy Astrophysical Phenomena Outflows/jets are ubiquitous in a wide range of astrophysical objects, yet the mechanisms responsible for their generation remain elusive. One hypothesis is that they are magnetically driven. Based on general relativistic MHD equations, we establish a formulation to describe the outflows driven by large-scale magnetic fields from the accretion disk in Schwarzschild spacetime. The outflow solution manifests as a contour level of a ``Bernoulli" function, which is determined by ensuring that it passes through both the slow and fast magnetosonic points. This approach is a general relativistic extension to the classical treatment of Cao and Spruit (1994). The initial plasma $β$ that permits magnetically driven outflow solutions is constrained, with the slow magnetosonic point above the footpoint setting an upper limit ($β_\mathrm{b}\lesssim 2$) and the Alfvén point inside the light cylinder setting a lower limit ($β_\mathrm{b}\gtrsim 0.02$). The higher the magnetization, the higher the temperature allowed, leading to relativistic outflows/jets. We investigate the relativistic outflows/jets of several typical objects such as active galactic nuclei (AGN), X-ray binaries (XRBs) and gamma-ray bursts (GRBs). The results indicate that all of these phenomena require strongly magnetized, high-temperature outflows as initial conditions, suggesting a potential association between the production of relativistic outflows/jets and corona-like structures. |
| title | The relativistic outflow driven by the large-scale magnetic field from an accretion disk |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2503.12135 |