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We model non-thermal emission spectrum of the extremely sub-Eddington X-raybinary system A0620-00. It is believed that this non-thermal emission isproduced by a radiatively inefficient "quiescent" accretion onto a stellar-massblack hole present in the system. We post-process GRMHD simulations withmultiwavelength, fully polarized, relativistic radiative transfer calculationsto predict broadband spectra and emission polarization levels for a range ofelectron models and accretion rates. We find that a model with strong couplingof electrons and ions in the accretion disk and accretion rate of only$\dot{M}=3\times10^{-13} [M_\odot yr^{-1}]$ is able to recover the observedX-ray spectral slope as well as the excess of linear polarization detected inthe source in NIR/optical bands. Our models constrain the spectral propertiesof a putative relativistic jet produced in this system. In addition we showthat the magnetized winds from our hot accretion flow carry away a smallfraction of the orbital angular momentum of the binary unable to explain theobserved rapid orbital decay of the system. Similar to the present GRMHDsimulations are often used to explain emission from sub-Eddington supermassvieblack holes in Sgr A* or M87; the present simulations allow us to test whethersome aspects of the quiescent black hole accretion are scale invariant.

Scale-invariance of black hole accretion: modeling emission from a black hole X-ray binary with relativistic accretion flow simulations