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We implement the KORAL code to perform two sets of very long generalrelativistic radiation magnetohydrodynamic simulations of an axisymmetricoptically thin magnetized flow around a non-rotating black hole: one with a newterm in the electromagnetic field tensor due to the radiation pressure felt bythe plasma electrons on the comoving frame of the electron-proton plasma, andone without. The source of the radiation is the accretion flow itself. Withoutthe new term, the system evolves to a standard accretion flow due to thedevelopment of the magneto-rotational instability (MRI). With the new term,however, the system eventually evolves to a magnetically arrested state (MAD)in which a large scale jet-like magnetic field threads the black hole horizon.Our results confirm the secular action of the Cosmic Battery in accretion flowsaround astrophysical black holes.

Numerical simulations of the Cosmic Battery in accretion flows around astrophysical black holes