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Wind-fed models offer a unique way to form predictive models of the accretionflow surrounding Sagittarius A*. We present 3D, wind-fed MHD and GRMHDsimulations spanning the entire dynamic range of accretion from parsec scalesto the event horizon. We expand on previous work by including nonzero blackhole spin and dynamically evolved electron thermodynamics. Initial conditionsfor these simulations are generated from simulations of the observed Wolf-Rayetstellar winds in the Galactic Centre. The resulting flow tends to be highlymagnetized ($\beta \approx 2$) with an $\sim$ $r^{-1}$ density profileindependent of the strength of magnetic fields in the winds. Our simulationsreach the MAD state for some, but not all cases. In tilted flows, SANE jetstend to align with the angular momentum of the gas at large scales, even ifthat direction is perpendicular to the black hole spin axis. Conversely, MADjets tend to align with the black hole spin axis. The gas angular momentumshows similar behavior: SANE flows tend to only partially align while MAD flowstend to fully align. With a limited number of dynamical free parameters, ourmodels can produce accretion rates, 230 GHz flux, and unresolved linearpolarization fractions roughly consistent with observations for several choicesof electron heating fraction. Absent another source of large-scale magneticfield, winds with a higher degree of magnetization (e.g., where the magneticpressure is 1/100 of the ram pressure in the winds) may be required to get asufficiently large RM with consistent sign.

Wind-Fed GRMHD Simulations of Sagittarius A*: Tilt and Alignment of Jets  and Accretion Discs, Electron Thermodynamics, and Multi-Scale Modeling of the  Rotation Measure