Coupling hydrodynamics and radiation calculations for star-jet interactions in AGN
Stellar populations can contribute to the non-thermal emission of radio-loud active galactic nuclei via the interaction with the relativistic jets. The shock produced between the stellar wind and the jet can accelerate particles and produce high-energy emission. We have performed 2D axisymmetric hyd...
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| Autores principales: | , , , , |
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| Formato: | Objeto de conferencia |
| Lenguaje: | Inglés |
| Publicado: |
2015
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| Materias: | |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/167853 |
| Aporte de: |
| Sumario: | Stellar populations can contribute to the non-thermal emission of radio-loud active galactic nuclei via the interaction with the relativistic jets. The shock produced between the stellar wind and the jet can accelerate particles and produce high-energy emission. We have performed 2D axisymmetric hydrodynamical simulations of the jet-stellar wind interaction and obtained the hydrodynamical properties of the emitting flow. With this information we study the evolution of the non-thermal particles accelerated in the collision and their IC and synchrotron radiation. We present here the results of these computations: detailed radiation maps and spectral energy distributions for di erent scenarios, depending on the position of the star in the jet, the magnetic field, and the viewing angle. We have studied two representative scenarios: the steady state of the jet-wind interaction; and the case in which a transient instability develops, enlarging the interaction region. |
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