Abstract
Puffy disc is a numerical model, expected to capture the properties of the accretion flow in X-ray black hole (BH) binaries in the luminous, mildly sub-Eddington state. We fit the kerrbb and kynbb spectral models in XSPEC to synthetic spectra of puffy accretion discs, obtained in general relativistic radiative magnetohydrodynamic simulations, to see if they correctly recover the BH spin and mass accretion rate assumed in the numerical simulation.
We conclude that neither of the two models is capable of correctly recovering the puffy disc parameters, which highlights a necessity to develop new, more accurate spectral models for the luminous regime of accretion in X-ray BH binaries. We propose that such spectral models should be based on the results of numerical simulations of accretion.