Modeling the inner part of M87 jet: confronting jet morphology with theory

TL;DR

This paper uses advanced simulations and radiative transfer calculations to compare theoretical jet formation models with actual observations of the M87 jet, finding the black hole spin-driven BZ-jet model best explains the observed morphology.

Contribution

It demonstrates that the BZ-jet model from a high-spin black hole can accurately reproduce observed jet features, bridging theory and observation.

Findings

BZ-jet model reproduces jet width and limb-brightening

Magnetic reconnection and kink instability influence jet morphology

High-spin black hole is consistent with observed jet structure

Abstract

The formation of jets in black hole accretion systems is a long-standing problem. It has been proposed that a jet can be formed by extracting the rotation energy of the black hole ("BZ-jet") or the accretion flow ("disk-jet"). While both models can produce collimated relativistic outflows, neither has successfully explained the observed jet morphology. In this paper, by employing general relativistic magnetohydrodynamic simulations, and considering nonthermal electrons accelerated by magnetic reconnection driven by kink instability of the jet, we have obtained images by radiative transfer calculations and compared them to millimeter observations of the jet in M87. We find that the BZ-jet originated from a magnetically arrested disk around a high-spin black hole can well reproduce the jet morphology, including its width and limb-brightening feature.