Inter--disks inversion surfaces
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arXiv
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| Format: | Preprint |
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2024
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| author | Pugliese, D. Stuchlik, Z. |
| author_facet | Pugliese, D. Stuchlik, Z. |
| contents | We consider a counter--rotating torus orbiting a central Kerr black hole (\textbf{BH}) with dimensionless spin $a$, and its accretion flow into the \textbf{BH}, in an agglomerate of an outer counter--rotating torus and an inner co--rotating torus. This work focus is the analysis of the inter--disks inversion surfaces. Inversion surfaces are spacetime surfaces, defined by the condition $u^ϕ=0$ on the flow torodial velocity, located out of the \textbf{BH} ergoregion, and totally embedding the \textbf{BH}. They emerge as a necessary condition, related to the spacetime frame--dragging, for the counter--rotating flows into the central Kerr \textbf{BH}. In our analysis we study the inversion surfaces of the Kerr spacetimes for the counter--rotating flow from the outer torus, impacting on the inner co--rotating disk. Being totally or partially embedded in (internal to) the inversion surfaces, the inner co--rotating torus (or jet) could be totally or in part ``shielded", respectively, from the impact with flow with $a u^ϕ<0$. We prove that, in general, in the spacetimes with $a<0.551$ the co--rotating toroids are always external to the accretion flows inversion surfaces. For $0.551<a<0.886$, co--rotating toroids could be partially internal (with the disk inner region, including the inner edge) in the flow inversion surface. For \textbf{BHs} with $a>0.886$, a co--rotating torus could be entirely embedded in the inversion surface and, for larger spins, it is internal to the inversion surfaces. Tori orbiting in the \textbf{BH} outer ergoregion are a particular case. Further constraints on the \textbf{BHs} spins are discussed in the article. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2410_03360 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Inter--disks inversion surfaces Pugliese, D. Stuchlik, Z. General Relativity and Quantum Cosmology High Energy Astrophysical Phenomena We consider a counter--rotating torus orbiting a central Kerr black hole (\textbf{BH}) with dimensionless spin $a$, and its accretion flow into the \textbf{BH}, in an agglomerate of an outer counter--rotating torus and an inner co--rotating torus. This work focus is the analysis of the inter--disks inversion surfaces. Inversion surfaces are spacetime surfaces, defined by the condition $u^ϕ=0$ on the flow torodial velocity, located out of the \textbf{BH} ergoregion, and totally embedding the \textbf{BH}. They emerge as a necessary condition, related to the spacetime frame--dragging, for the counter--rotating flows into the central Kerr \textbf{BH}. In our analysis we study the inversion surfaces of the Kerr spacetimes for the counter--rotating flow from the outer torus, impacting on the inner co--rotating disk. Being totally or partially embedded in (internal to) the inversion surfaces, the inner co--rotating torus (or jet) could be totally or in part ``shielded", respectively, from the impact with flow with $a u^ϕ<0$. We prove that, in general, in the spacetimes with $a<0.551$ the co--rotating toroids are always external to the accretion flows inversion surfaces. For $0.551<a<0.886$, co--rotating toroids could be partially internal (with the disk inner region, including the inner edge) in the flow inversion surface. For \textbf{BHs} with $a>0.886$, a co--rotating torus could be entirely embedded in the inversion surface and, for larger spins, it is internal to the inversion surfaces. Tori orbiting in the \textbf{BH} outer ergoregion are a particular case. Further constraints on the \textbf{BHs} spins are discussed in the article. |
| title | Inter--disks inversion surfaces |
| topic | General Relativity and Quantum Cosmology High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2410.03360 |