In nearby active galactic nuclei (AGNs), spectra of continuum and/or lines in ALMA provide information that reveals pc-scale gas structures. We investigate how the dynamical structure of the gas can explain the observed multi-wavelength radiation field based on numerical simulations. Wada (2012, 2015) suggested the radiative fountain model indicating that the geometrically and optically thick torus in the AGN unified model is formed by the dusty outflow from the dust radiative force. This dynamical model successfully explains infrared dust radiation (Wada et al. 2016) and ionized absorption lines of X-rays (Ogawa et al. 2022). In this talk, I will discuss the contribution of the continuum from ionized gas of free-free emission and dusty gas of thermal dust emission in the AGN torus, in addition to the multi-phase outflow by ionized emission lines and the accretion process by absorption lines, by comparing dynamical simulation models with the ALMA observations.