Ray-Tracing in Relativistic Jet Simulations: A Polarimetric Study of Magnetic Field Morphology and Electron Scaling Relations
arXiv:2109.03514 · doi:10.1051/0004-6361/202141454
Abstract
The jets emanating from the centers of active galactic nuclei (AGN) are among the most energetic objects in the universe. Investigating how the morphology of the jet's synchrotron emission depends on the magnetic nature of the jet's relativistic plasma is fundamental to the comparison between numerical simulations and the observed polarization of relativistic jets. Through the use of 3D relativistic magnetohydrodynamic (RMHD) jet simulations (computed using the PLUTO code) we study how the jet's synchrotron emission depends upon the morphology of the jet's magnetic field structure. Through the application of polarized radiative transfer and ray-tracing (via the RADMC-3D code) we create synthetic radio maps of the jet's total intensity as well as the linearly and circularly polarized intensity for each jet simulation. In particular, we create synthetic ray-traced images of the jet's polarized synchrotron emission when the jet carries a predominantly poloidal, helical, and toroidal magnetic field. We also explore several scaling relations in which the underlying electron power-law distribution is set proportional to: (i) the jet's thermal plasma density, (ii) the jet's internal energy density, and (iii) the jet's magnetic energy density. We find that: (i) the jet emission is edge brightened when the magnetic field is toroidal in nature and spine brightened when the magnetic field is poloidal in nature, (ii) the circularly polarized emission exhibits both negative and positive signs for the toroidal magnetic field morphology at an inclination of 45° as well as 5°, and (iii) the relativistic jet's emission is largely independent of different emission scaling relations when the ambient medium is excluded.
arXiv comment17 pages, 92 figures, Accepted for publication in A&A
References in corpus (29)
- PLUTO: a Numerical Code for Computational Astrophysics
- Relativistic Reconnection: an Efficient Source of Non-Thermal Particles
- The extent of power-law energy spectra in collisionless relativistic magnetic reconnection in pair plasmas
- Polarization and structure of relativistic parsec-scale AGN jets
- The Piecewise Parabolic Method for Multidimensional Relativistic Fluid Dynamics
- An HLLC Solver for Relativistic Flows -- II. Magnetohydrodynamics
- A wide and collimated radio jet in 3C 84 on the scale of a few hundred gravitational radii
- A five-wave HLL Riemann solver for relativistic MHD
- Synchrotron radiation of self-collimating relativistic MHD jets
- Catching the Radio Flare in CTA 102 III. Core-Shift and Spectral Analysis
- Three dimensional magnetic field structure of six parsec-scale active galactic nuclei jets
- A Particle Module for the PLUTO code: II - Hybrid Framework for Modeling Non-thermal emission from Relativistic Magnetized flows
- Reconnection-driven particle acceleration in relativistic shear flows
- MOJAVE: Monitoring of Jets in AGN with VLBA Experiments - II. First-Epoch 15 GHz Circular Polarization Results
- Particle acceleration in astrophysical jets
- Spatial growth of current-driven instability in relativistic rotating jets and the search for magnetic reconnection
- Determining the Dominant Acceleration Mechanism during Relativistic Magnetic Reconnection in Large-scale Systems
- Disks and Jets - Gravity, Rotation and Magnetic Fields
- Spectral evolution of flaring blazars from numerical simulations
- High Levels of Circularly Polarized Emission from the Radio Jet in NGC 1275 (3C 84)
- Spatially resolved origin of mm-wave linear polarization in the nuclear region of 3C 84
- GRMHD/RMHD Simulations and Stability of Magnetized Spine-Sheath Relativistic Jets
- MHD simulations of three-dimensional Resistive Reconnection in a cylindrical plasma column
- Fast magnetic reconnection structures in Poynting-flux dominated jets
- The 15--43-GHz Parsec-scale Circular Polarization of 41 Active Galactic Nuclei
- Pinpointing the jet apex of 3C 84
- The Jets of AGN as giant co-axial cables
- Faraday Conversion in Turbulent Blazar Jets
- The TANAMI Program