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| Format: | Preprint |
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2024
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| Online-Zugang: | https://arxiv.org/abs/2405.00097 |
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| author | Paraschos, G. F. Debbrecht, L. C. Kramer, J. A. Traianou, E. Liodakis, I. Krichbaum, T. P. Kim, J. -Y. Janssen, M. Nair, D. G. Savolainen, T. Ros, E. Bach, U. Hodgson, J. A. Lisakov, M. MacDonald, N. R. Zensus, J. A. |
| author_facet | Paraschos, G. F. Debbrecht, L. C. Kramer, J. A. Traianou, E. Liodakis, I. Krichbaum, T. P. Kim, J. -Y. Janssen, M. Nair, D. G. Savolainen, T. Ros, E. Bach, U. Hodgson, J. A. Lisakov, M. MacDonald, N. R. Zensus, J. A. |
| contents | The spatial scales of relativistic radio jets, probed by relativistic magneto-hydrodynamic jet launching simulations (RMHDs) and by most very-long-baseline interferometry (VLBI) observations differ by an order of magnitude. Bridging the gap between these RMHD simulations and VLBI observations requires selecting nearby active galactic nuclei (AGN), the parsec-scale region of which can be resolved. 3C 84 is a nearby bright AGN fulfilling the necessary requirements: it is launching a powerful, relativistic jet powered by a central supermassive black hole, while also being very bright. Using 22 GHz global VLBI measurements of 3C 84 we aim to study its sub-parsec region in both total intensity and linear polarisation, to explore the properties of this jet, with a linear resolution of $\sim0.1$ parsec. We test different simulation setups by altering the bulk Lorentz factor $Γ$ of the jet, as well as the magnetic field configuration (toroidal, poloidal, helical). We confirm the persistence of a limb brightened structure, which reaches deep into the sub-parsec region. The corresponding electric vector position angles (EVPAs) follow the bulk jet flow inside but tend to be orthogonal to it near the edges. Our state-of-the-art RMHD simulations show that this geometry is consistent with a spine-sheath model, associated with a mildly relativistic flow and a toroidal magnetic field configuration. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_00097 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Evidence for a toroidal magnetic field in the core of 3C 84 Paraschos, G. F. Debbrecht, L. C. Kramer, J. A. Traianou, E. Liodakis, I. Krichbaum, T. P. Kim, J. -Y. Janssen, M. Nair, D. G. Savolainen, T. Ros, E. Bach, U. Hodgson, J. A. Lisakov, M. MacDonald, N. R. Zensus, J. A. High Energy Astrophysical Phenomena Astrophysics of Galaxies The spatial scales of relativistic radio jets, probed by relativistic magneto-hydrodynamic jet launching simulations (RMHDs) and by most very-long-baseline interferometry (VLBI) observations differ by an order of magnitude. Bridging the gap between these RMHD simulations and VLBI observations requires selecting nearby active galactic nuclei (AGN), the parsec-scale region of which can be resolved. 3C 84 is a nearby bright AGN fulfilling the necessary requirements: it is launching a powerful, relativistic jet powered by a central supermassive black hole, while also being very bright. Using 22 GHz global VLBI measurements of 3C 84 we aim to study its sub-parsec region in both total intensity and linear polarisation, to explore the properties of this jet, with a linear resolution of $\sim0.1$ parsec. We test different simulation setups by altering the bulk Lorentz factor $Γ$ of the jet, as well as the magnetic field configuration (toroidal, poloidal, helical). We confirm the persistence of a limb brightened structure, which reaches deep into the sub-parsec region. The corresponding electric vector position angles (EVPAs) follow the bulk jet flow inside but tend to be orthogonal to it near the edges. Our state-of-the-art RMHD simulations show that this geometry is consistent with a spine-sheath model, associated with a mildly relativistic flow and a toroidal magnetic field configuration. |
| title | Evidence for a toroidal magnetic field in the core of 3C 84 |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2405.00097 |