The rebrightening SED of MAXI J1820+070 is best explained by a radiatively inefficient accretion flow at mdot ~ 1e-3, a separate jet power-law component, and a cool outer H-alpha emitting region.
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Multiwavelength Observations of the Black Hole X-ray Binary MAXI J1820$+$070 in the Rebrightening Phase
The rebrightening SED of MAXI J1820+070 is best explained by a radiatively inefficient accretion flow at mdot ~ 1e-3, a separate jet power-law component, and a cool outer H-alpha emitting region.