Comprehensive analysis of magnetospheric gaps around Kerr black holes using 1D GRPIC simulations

Abstract

Spark gaps are likely the source of plasma in active black hole (BH) magnetospheres. In this paper, we present results of 1D general-relativistic particle-in-cell simulations of a starved BH magnetosphere with a realistic treatment of inverse Compton scattering and pair production, for a broad range of conditions, run times longer than in previous studies, and different setups. We find that following the initial discharge, the system undergoes gradual evolution over prolonged time until either, restoring the vacuum state or reaching a state of quasi-periodic oscillations, depending on the spectral shape and luminosity of the ambient radiation field. The oscillations occur near the null charge surface in cases where the global magnetospheric current is in the direction defined by the product of the asymptotic Goldreich-Julian charge density and the radial velocity, while they occur near the boundary of the simulation box when it is the opposite direction (return current). Their amplitude and the resultant luminosity of TeV photons emitted from the gap depend sensitively on the conditions; for the cases studied here the ratio of TeV luminosity to the Blandford-Znajek power ranges from 10 −5 to 10 −2 , suggesting that strong flares may be generated by moderate changes in disk emission. We also examined the dependence of the solution on the initial number of particles per cell (PPC) and found convergence for PPC of about 50 for the cases examined. At lower PPC values the pair multiplicity is found to be artificially high, affecting the solution considerably.

Synthetic gamma-ray lightcurves of Kerr black-hole magnetospheric activity from particle-in-cell simulations

“…If of magnetospheric origin, rather being a manifestation of the intrinsic variability due to the pair production mechanism, flares could be interpreted as the fast response of a black-hole magnetosphere to a sudden change in the external parameters. This conclusion was also reached by Levinson & Cerutti (2018) and Kisaka et al (2020), through radiative 1D GRPIC simulations. For example, a variation in the accretion rate would cause the density of soft photons to increase, leading to an increase in τ 0 .…”

A Jet-Bases Emission Model of the EHT 2017 Image of M87*

“…In the funnel region, particle outflows are thought to originate from the stagnation surface, below which the particles fall by the BH gravity (Takahashi et al 1990;Pu et al 2015). This picture of the funnel is based on MHD, whereas the MHD condition might be broken in some parts at/below the stagnation surface (e.g., Broderick & Tchekhovskoy 2015;Hirotani & Pu 2016;Kisaka et al 2020). Such inner regions of jets have not been probed by any observation.…”