A HYDRODYNAMICAL MECHANISM FOR GENERATING ASTROPHYSICAL JETS
Whenever in a classical accretion disk the thin disk approximation fails inte- rior to a certain radius, a transition from Keplerian to radial infalling trajectories should occur. We show that this transition is actually expected to occur inte- rior to a certain critical radius, provided surface den...
| Autores: | , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2014 |
| País: | México |
| Institución: | Universidad Nacional Autónoma de México |
| Repositorio: | Redalyc-UNAM |
| OAI Identifier: | oai:redalyc.org:57131044004 |
| Acceso en línea: | https://www.redalyc.org/articulo.oa?id=57131044004 |
| Access Level: | acceso abierto |
| Palabra clave: | Física, Astronomía y Matemáticas Accretion jets — ISM jets and outflows accretion disks — hydrodynamics — galaxies |
| Sumario: | Whenever in a classical accretion disk the thin disk approximation fails inte- rior to a certain radius, a transition from Keplerian to radial infalling trajectories should occur. We show that this transition is actually expected to occur inte- rior to a certain critical radius, provided surface density profiles are steeper than Σ(R) ∝ R−1/2 , and further, that it probably corresponds to the observationally inferred phenomena of thick hot walls internally limiting the extent of many stellar accretion disks. Infalling trajectories will lead to the convergent focusing and con- centration of matter towards the very central regions, most of which will simply be swallowed by the central object. We show through a perturbative hydrodynamical analysis, that this will naturally develop a well collimated pair of polar jets. A first analytic treatment of the problem described is given, proving the feasibility of purely hydrodynamical mechanisms for astrophysical jet generation. |
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