Modeling the high resolution X-ray spectrum of Sgr A* in quiescence

Despite being the closest supermassive black hole (SMBH), Sgr A*’s accretion is not well understood. The SMBH is accreting at ≈10^-9 L_edd, 10⁵ times lower than the rate expected from Bondi accretion alone. This poses challenges for understanding accretion physics in the galactic center. Many works have investigated the spectrum by fitting it with radiatively inefficient accretion flow (RIAF) models, assuming standard temperature-density profiles. We fit the high resolution X-ray spectrum of Sgr A* extracted from 3 Ms of Chandra data obtained through the Galactic Center X-ray Visionary Program. We use RIAF models along with temperature-density profiles from simulations of outflows from nearby Wolf-Rayet stars (Calderon et al. 2020) that feed the SMBH. We present preliminary results of our modeling.