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Substructures in Simulations of Relativistic Jet Formation

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Abstract

We present a set of simulations of relativistic jets from accretion disk initial setup with numerical solutions of a system of general-relativistic magnetohydrodynamics (GRMHD) partial differential equations in a fixed black hole (BH) spacetime which is able to show substructures formations inside the jet as well as lobe formation on the jet head. For this, we used a central scheme of finite volume method without dimensional split and with no Riemann solvers namely the Nessyahu-Tadmor method. Thus, we were able to obtain stable numerical solutions with spurious oscillations under control and with no excessive numerical dissipation. Therefore, we developed some setups for initial conditions capable of simulating the formation of relativistic jets from the accretion disk falling onto central black hole until its ejection, both immersed in a magnetosphere. In our simulations, we were able to observe some substructure of a jet created from an accretion initial disk, namely, jet head, knots, cocoon, and lobe. Also, we present an explanation for cocoon formation and lobe formation. Each initial scenario was determined by ratio between disk density and magnetosphere density, showing that this relation is very important for the shape of the jet and its substructures.

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Authors and Affiliations

  1. Institute of Mathematics, Statistics and Scientific Computing, University State of Campinas (UNICAMP), 651 Sérgio Buarque de Holanda street, University City, 13083-859, Campinas, SP, Brazil

    Raphael de Oliveira Garcia & Samuel Rocha de Oliveira

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  1. Raphael de Oliveira Garcia
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  2. Samuel Rocha de Oliveira
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Correspondence to Raphael de Oliveira Garcia.

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Garcia, R.d.O., Oliveira, S.R.d. Substructures in Simulations of Relativistic Jet Formation. Braz J Phys 47, 197–214 (2017). https://doi.org/10.1007/s13538-017-0489-9

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  • DOI: https://doi.org/10.1007/s13538-017-0489-9

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