Direct time radio variability induced by non-axisymmetric standing accretion shock instability: implications for M87

TL;DR

This paper demonstrates the first direct simulation of time-variable radio images caused by non-axisymmetric shock instabilities in black hole accretion flows, with implications for observing M87's dynamic environment.

Contribution

It introduces a general relativistic simulation of shock-induced radio variability around black holes, linking theoretical models with potential future observations of M87.

Findings

Predicted radio images show variability near 15 Schwarzschild radii.

Results align with existing radio spectra and VLBA observations of M87.

Suggests detectability of variability with future space telescopes.

Abstract

We show for the first time the direct time variable radio images in the context of shocked accretion flows around a black hole under the general relativistic treatment of both hydrodynamics and radiation transfer. Time variability around a black hole can be induced by the non-axisymmetric standing accretion shock instability (namely Black Hole SASI). Since the spiral arm shock waves generate the density and temperature waves at the post shock region, they cause time variability in the black hole vicinity. Based on our dynamical simulations, we discuss a possibility of detection for the time variable radio images of M87 by the future space telescope VSOP2/ASTRO-G satellite. The most luminous part of the images is predicted to be near 15 Schwarzschild radii for some snapshots. We show that our results are consistent with existing observational data such as timeaveraged radio spectra, VLBA images and variability timescale for M87. We also discuss observations of M87 with millimeter and sub-millimeter interferometers.