Existence of a persistent jet in Sgr A*

Determine whether Sagittarius A* hosts a persistent relativistic jet, rather than an outflow produced by winds or by the complex morphology of its accretion flow.

Background

The paper models the accelerated protons as a proton-dominated outflow powered by the magnetic Penrose process and estimates its kinetic power. However, the authors note that no conclusive observational evidence currently establishes the presence of a persistent jet from Sagittarius A*. Various radio, X-ray, and kinematic structures have been interpreted as possible signatures of a weak collimated outflow, while alternative explanations involving winds or accretion-flow morphology remain viable.

Resolving this issue is important for interpreting the calculated kinetic powers and for determining whether the predicted magnetic-Penrose-process outflow corresponds to a physically existing jet or only to a theoretical proton outflow.