Radiative Signatures of Parsec-Scale Magnetised Jets
Relativistic jets are launched from the immediate vicinity of black holes and can reach kilo-parsec scales. During their evolution from the smallest to the largest scales, they encounter different physical conditions (e.g., ambient configurations and magnetic fields) which can modify their morpholog...
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doaj-585c7cd74cbb4f77b0794d1305e2d8c12020-11-24T21:43:36ZengMDPI AGGalaxies2075-44342017-11-01547310.3390/galaxies5040073galaxies5040073Radiative Signatures of Parsec-Scale Magnetised JetsChristian M. Fromm0Oliver Porth1Ziri Younsi2Yosuke Mizuno3Mariafelica de Laurentis4Hector Olivares5Luciano Rezzolla6Institut für Theoretische Physik, Goethe Universität, Max-von-Laue-Str. 1, D-60438 Frankfurt, GermanyInstitut für Theoretische Physik, Goethe Universität, Max-von-Laue-Str. 1, D-60438 Frankfurt, GermanyInstitut für Theoretische Physik, Goethe Universität, Max-von-Laue-Str. 1, D-60438 Frankfurt, GermanyInstitut für Theoretische Physik, Goethe Universität, Max-von-Laue-Str. 1, D-60438 Frankfurt, GermanyInstitut für Theoretische Physik, Goethe Universität, Max-von-Laue-Str. 1, D-60438 Frankfurt, GermanyInstitut für Theoretische Physik, Goethe Universität, Max-von-Laue-Str. 1, D-60438 Frankfurt, GermanyInstitut für Theoretische Physik, Goethe Universität, Max-von-Laue-Str. 1, D-60438 Frankfurt, GermanyRelativistic jets are launched from the immediate vicinity of black holes and can reach kilo-parsec scales. During their evolution from the smallest to the largest scales, they encounter different physical conditions (e.g., ambient configurations and magnetic fields) which can modify their morphology and dynamics. Using state-of-the-art relativistic magneto-hydrodynamical simulations and ray-tracing algorithms, we model the dynamics of jets along with their radiation microphysics, investigating the impact of magnetisation on the jet dynamics and the observed emission. During the post-processing procedure we account for the properties of the observing array (sparse uv-plane) and the imaging algorithm, enabling a more direct comparison between simulations and ground-or space-based very-long-baseline interferometry (VLBI) observations. The different jet models can be distinguished from the reconstructed radio images.https://www.mdpi.com/2075-4434/5/4/73relativistic jetsspecial relativistic magneto-hydrodynamicsnon-thermal emissionVLBI |
collection |
DOAJ |
language |
English |
format |
Article |
sources |
DOAJ |
author |
Christian M. Fromm Oliver Porth Ziri Younsi Yosuke Mizuno Mariafelica de Laurentis Hector Olivares Luciano Rezzolla |
spellingShingle |
Christian M. Fromm Oliver Porth Ziri Younsi Yosuke Mizuno Mariafelica de Laurentis Hector Olivares Luciano Rezzolla Radiative Signatures of Parsec-Scale Magnetised Jets Galaxies relativistic jets special relativistic magneto-hydrodynamics non-thermal emission VLBI |
author_facet |
Christian M. Fromm Oliver Porth Ziri Younsi Yosuke Mizuno Mariafelica de Laurentis Hector Olivares Luciano Rezzolla |
author_sort |
Christian M. Fromm |
title |
Radiative Signatures of Parsec-Scale Magnetised Jets |
title_short |
Radiative Signatures of Parsec-Scale Magnetised Jets |
title_full |
Radiative Signatures of Parsec-Scale Magnetised Jets |
title_fullStr |
Radiative Signatures of Parsec-Scale Magnetised Jets |
title_full_unstemmed |
Radiative Signatures of Parsec-Scale Magnetised Jets |
title_sort |
radiative signatures of parsec-scale magnetised jets |
publisher |
MDPI AG |
series |
Galaxies |
issn |
2075-4434 |
publishDate |
2017-11-01 |
description |
Relativistic jets are launched from the immediate vicinity of black holes and can reach kilo-parsec scales. During their evolution from the smallest to the largest scales, they encounter different physical conditions (e.g., ambient configurations and magnetic fields) which can modify their morphology and dynamics. Using state-of-the-art relativistic magneto-hydrodynamical simulations and ray-tracing algorithms, we model the dynamics of jets along with their radiation microphysics, investigating the impact of magnetisation on the jet dynamics and the observed emission. During the post-processing procedure we account for the properties of the observing array (sparse uv-plane) and the imaging algorithm, enabling a more direct comparison between simulations and ground-or space-based very-long-baseline interferometry (VLBI) observations. The different jet models can be distinguished from the reconstructed radio images. |
topic |
relativistic jets special relativistic magneto-hydrodynamics non-thermal emission VLBI |
url |
https://www.mdpi.com/2075-4434/5/4/73 |
work_keys_str_mv |
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1725913162234986496 |