Modeling the inner part of M87 jet: confronting jet morphology with theory
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.
Keywords
Cite
@article{arxiv.2206.05661,
title = {Modeling the inner part of M87 jet: confronting jet morphology with theory},
author = {Hai Yang and Feng Yuan and Hui Li and Yosuke Mizuno and Fan Guo and Rusen Lu and Luis C. Ho and Jieshuang Wang},
journal= {arXiv preprint arXiv:2206.05661},
year = {2024}
}
Comments
We would like to submit a new article with the same research question as this article. We have made significant modifications in the following two aspects. We have constructed a more refined and accurate theoretical model and greatly improved the resolution of the simulation. Republishing a new version avoids confusion and misleading readers