2015/12/16 by R.O. Garcia, R. O. Garcia, Garcia, R. O. +3
Physics and Astronomy · #65Z05 #76W05 #83-04 #83-08 #83C10 #83C55 #83C57 #Astrophysical Phenomena and Observations #Astrophysics and Cosmic Phenomena #FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc) #High Energy Astrophysical Phenomena (astro-ph.HE) #Pulsars and Gravitational Waves Research #astro-ph.HE #gr-qc #msc:65Z05 #msc:76W05 #msc:83-04 #msc:83-08 #msc:83C10 #msc:83C55 #msc:83C57
paper · pdf · doi:10.48550/arxiv.1602.02143
12 pages, 20 figures
arxiv created 2015/12/16 · openalex publication_date 2015/12/16 · arxiv updated 2016/02/08 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We present a set of simulations of relativistic jets from accretion disk initial setup with a new code in Fortran 90 to get 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 a lobe formation on the disk. For this, a central scheme of finite volume method without dimensional split and no Riemann solvers (a Nessyahu-Tadmor method) was implemented. Thus, we were able to obtain stable numerical solutions with spurious oscillations under control and no excessive numerical dissipation. We setup a magnetized accretion disk uncharged plasma surrounding a central Schwarzschild BH immersed in a magnetosphere which evolve to the ejection of matter in the form of jet with its substructures over a distance of almost twenty times the BH radius.