Simulations of Jets from Active Galactic Nuclei and Gamma‐Ray Bursts

Aloy, M. Á.; Mimica, P.

doi:10.1002/9783527641741.ch10

Cited by 3 publications

(2 citation statements)

References 225 publications

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“…Recently, it has become possible to study jets with relativistic 3-D hydrodynamic (HD) and magnetohydrodynamic (MHD) codes (see e.g. [39,40] and references therein). The simulations can reproduce the observed morphologies of radio sources rather well.…”

Section: Magnetohydrodynamic Simulations Of Jetsmentioning

confidence: 99%

Active galactic nuclei — the physics of individual sources and the cosmic history of formation and evolution

Krawczynski

Treister

2013

Front. Phys.

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In this paper we give a brief review of the astrophysics of active galactic nuclei (AGN). After a general introduction motivating the study of AGNs, we discuss our present understanding of the inner workings of the central engines, most likely accreting black holes with masses between 10 6 and 10 10 M . We highlight recent results concerning the jets (collimated outflows) of AGNs derived from X-ray observations (Chandra) of kpc-scale jets and γ-ray observations of AGNs (Fermi, Cherenkov telescopes) with jets closely aligned with the lines of sight (blazars), and discuss the interpretation of these observations. Subsequently, we summarize our knowledge about the cosmic history of AGN formation and evolution. We conclude with a description of upcoming observational opportunities. MotivationActive galactic nuclei (AGNs) are galaxies that harbor supermassive black holes (SMBHs) of a few million to a few billion solar masses. Whereas it seems likely that all galaxies contain one or more supermassive black holes [1,2], the black holes in AGNs give rise to spectacular observational consequences because they accrete matter and convert the gravitational energy of the accreted matter (and possibly also the rotational energy of the black hole) into mechanical and electromagnetic energy. A few of the most salient motivations for the study of AGNs are: and statistical characterization. The study of AGNs in the nearby Universe shows that the diversity of AGNs can be understood as resulting from observing a smaller number of basic AGN types from different viewing angles (see Section 3.1).Accretion Physics: AGNs are powered by the accretion of magnetized plasma. Studies of AGN accretion flows complement studies of other accretion flows in astrophysics: accretion onto protostars and stars, accretion onto compact stellar remnants (neutron stars and stellar mass black holes), and the accretion that powers gamma-ray bursts. One goal of the studies of AGN accretion flows is to provide a physical explanation of the different types of AGNs and their states in terms of the nature of their accretion flows and environments (see Section 3.3).Role in Eco-Systems: AGNs play an important role for galactic and galaxy cluster eco-systems, i.e. their mechanical and electromagnetic power contributes to the heating of the interstellar and intracluster medium, and thus influences the star formation of the host systems (see Section 2.4).History through Cosmic Time: Deep radio, IR, optical and X-ray observations of AGNs have provided us with a wealth of information about the cosmic history of the formation and growth of supermassive black holes and the evolution of AGNs. Related areas of research are to clarify the role of AGNs in re-ionizing the intergalactic medium, and to explain the correlation between black hole masses and the properties of the host galaxy observed in the local Universe (see Sections 4 & 5).Fundamental Physics: On the most fundamental level, AGNs allow us to test the theory of general relativity (GR). GR's no-hair theor...

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Section: Magnetohydrodynamic Simulations Of Jetsmentioning

confidence: 99%

Active galactic nuclei — the physics of individual sources and the cosmic history of formation and evolution

Krawczynski

Treister

2013

Front. Phys.

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“…MRGENESIS uses operator-splitting, finite-volumes, explicit method and employs approximate Riemann solvers for the computation of intercell fluxes, as well as total variation diminishing second and third-order Runge-Kutta methods for the time integration (for a recent overview of jet simulation codes see e.g. [8]). MRGENESIS has been massively parallelized using OpenMP and MPI libraries and has achieved reasonable scaling up to 10 4 cores on the MareNostrum machine at the Barcelona Supercomputing Centre.…”

Section: Special Relativistic Magnetohydrodynamicsmentioning

confidence: 99%

Numerical simulations of dynamics and emission from relativistic astrophysical jets

Mimica

Aloy

Rueda-Becerril

et al. 2013

J. Phys.: Conf. Ser.

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Abstract. Broadband emission from relativistic outflows (jets) of active galactic nuclei (AGN) and gamma-ray bursts (GRBs) contains valuable information about the nature of the jet itself and about the central engine which launches it. Using special relativistic hydrodynamics and magnetohydrodynamics simulations we study the dynamics of the jet and its interaction with the surrounding medium. The observational signature of the simulated jets is computed using a radiative transfer code developed specifically for the purpose of computing multi-wavelength, time-dependent, non-thermal emission from astrophysical plasmas. We present results of a series of long-term projects devoted to understanding the dynamics and emission of jets in parsec-scale AGN jets, blazars and the afterglow phase of the GRBs.

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CAFE-R: A Code That Solves the Special Relativistic Radiation Hydrodynamics Equations

Rivera-Paleo

Guzmán

2019

ApJS

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We present a 3D special-relativistic radiation hydrodynamics code. It uses the radiative inversion scheme with the M1-closure relation for the radiation equations, which allows the treatment of a wide range of optical depth, temperature and opacity. The radiation field is treated in the grey-body approximation. We present the standard 1D and 2D tests that include both optically thin and thick scenarios, as well as hydrodynamical and radiation pressure dominated configurations. As an application in 3D, we show the evolution of a jet driven by radiation-hydrodynamics with a helical perturbation. The code is expected to allow the exploration of scenarios in high-energy astrophysics where the radiation is important, like sources of GRBs.

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Simulations of Jets from Active Galactic Nuclei and Gamma‐Ray Bursts

Cited by 3 publications

References 225 publications

Active galactic nuclei — the physics of individual sources and the cosmic history of formation and evolution

Active galactic nuclei — the physics of individual sources and the cosmic history of formation and evolution

Numerical simulations of dynamics and emission from relativistic astrophysical jets

CAFE-R: A Code That Solves the Special Relativistic Radiation Hydrodynamics Equations

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