VHE Emission from Magnetic Reconnection in the RIAF of SgrA*

Understand

The cosmic-ray (CR) accelerator at the galactic centre (GC) is not yet established by current observations.

• Here we investigate the radiative-inefficient accretion flow (RIAF) of Sagittarius A* (SgrA*) as a CR accelerator assuming acceleration by turbulent magnetic reconnection, and derive possible emission fluxes of CRs interacting within the RIAF (the central $\sim10^{13}$cm).
• The target environment of the RIAF is modelled with numerical, general relativistic magneto-hydrodynamics (GRMHD) together with leptonic radiative transfer simulations.
• The acceleration of the CRs is not computed here.