The Mass-Radius (M–R) relation for a sample of 47 moderately magnetized white dwarfs (WD) is presented. Instead of traditional methods for deriving the mass and radius, we have used their location in the Hertzsprung-Russel diagram to estimate their masses. The atmospheric parameters, effective temperature (T \(_{eff}\) ), surface gravity (log g), and luminosity, are first derived by the Virtual Observatory Spectral Energy Distribution Analyzer (VOSA). The observed M–R relation is then compared with theoretical predictions from finite temperature models considering different magnetic field strengths. The agreement between the observations and model prediction at lower field strength may suggest the existence of Super-Chandrasekhar White dwarfs at stronger fields.