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Quantifying coronal magnetic field remains a central problem in solarphysics. Nowadays the coronal magnetic field is often modelled using nonlinearforce-free field (NLFFF) reconstructions, whose accuracy has not yet beencomprehensively assessed. Here we perform a detailed casting of the NLFFFreconstruction tools, such as pi-disambiguation, photospheric fieldpreprocessing, and volume reconstruction methods using a 3D snapshot of thepublicly available full-fledged radiative MHD model. Specifically, from the MHDmodel we know the magnetic field vector in the entire 3D domain, which enablesus to perform "voxel-by-voxel" comparison of the restored and the true magneticfield in the 3D model volume. Our tests show that the availablepi-disambiguation methods often fail at the quiet sun areas dominated bysmall-scale magnetic elements, while they work well at the AR photosphere and(even better) chromosphere. The preprocessing of the photospheric magneticfield, although does produce a more force-free boundary condition, also resultsin some effective `elevation' of the magnetic field components. This`elevation' height is different for the longitudinal and transverse components,which results in a systematic error in absolute heights in the reconstructedmagnetic data cube. The extrapolations performed starting from actual ARphotospheric magnetogram are free from this systematic error, while have othermetrics comparable with those for extrapolations from the preprocessedmagnetograms. This finding favors the use of extrapolations from the originalphotospheric magnetogram without preprocessing. Our tests further suggest thatextrapolations from a force-free chromospheric boundary produce measurablybetter results, than those from the photospheric boundary.

Casting the Coronal Magnetic Field Reconstruction Tools in 3D Using MHD Bifrost Model