http://arxiv.org/abs/2205.08729
We explore the formation, energetics and geometry of the jets and variability of their central engine by means of 3D general relativistic magneto-hydrodynamical simulations of the magnetically arrested disk accretion in Kerr geometry. We study both fast and slowly rotating black holes, and address our simulations to both active galaxy centers and Gamma Ray Burst engines. The structured jets are postulated to account for emission properties of high energy sources across the mass scale, launched from stellar mass black holes in GRBs and from supermassive black holes in AGN. Their active cores contain magnetized accretion disks and rotation of the Kerr black hole provides mechanism for launching relativistic jets. This process works most effectively if the mode of accretion turns out to be magnetically arrested. In this mode, the modulation of jets launched from the engine is related to internal instabilities in the accretion flow, that work on smallest time and spatial scales. As these scales are related to the light crossing time, and the black hole gravitational radius, the universal model of jet-disk connection should scale with the mass of the black hole. The system evolution is governed by the physical parameters of the engine, such as the black hole spin, and disk size, as well as disk magnetisation. We find that stronger magnetic fields may lead to jet quenching. The effect is supposed to be important mainly for Gamma Ray Burst jets and may be related to the magnetically driven winds from their engines.
A. Janiuk and B. James
Thu, 19 May 22
34/61
Comments: 18 pages; 10 figures;submitted to ApJ
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