TL;DR
This paper explores the AGN jet model as a plausible explanation for the Fermi bubbles, using hydrodynamic simulations to match observed bubble features and discussing potential issues and future directions.
Contribution
It presents hydrodynamic simulations supporting the AGN jet model for Fermi bubbles and discusses how shear viscosity can suppress instabilities at the bubble surface.
Findings
Simulations reproduce the location and shape of Fermi bubbles.
Shear viscosity helps suppress interface instabilities.
The model aligns with analogies to radio lobes in galaxies.
Abstract
The nature and origin of the Fermi bubbles detected in the inner Galaxy remain elusive. In this paper, we briefly discuss some recent theoretical and observational developments, with a focus on the AGN jet model. Analogous to radio lobes observed in massive galaxies, the Fermi bubbles could be naturally produced by a pair of opposing jets emanating nearly along the Galaxy's rotation axis from the Galactic center. Our two-fluid hydrodynamic simulations reproduce quite well the bubble location and shape, and interface instabilities at the bubble surface could be effectively suppressed by shear viscosity. We briefly comment on some potential issues related to our model, which may lead to future progress.
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