A self-similar magnetohydrostatic model of solar faculae is presented. The model is based on the Schlueter-Temesvary equation, originally derived for sunspots. Magnetic tension and twisted magnetic field are taken into account. The exact magnetohydrostatic solution obtained from an observationally derived pressure deficit basically confirms Chapman's semiempirical facular model without tension. The difference between a facula and a sunspot and the thermodynamic consequences of a twisted magnetic field are discussed. Pressure and temperature profiles at different heights are presented.