Abstract: The solar corona is hot and tenuous. Yet, it hosts a variety of mysteriously cool and dense plasmas in two distinct forms: prominences and coronal rain. What  they have in common is catastrophic radiative cooling of hot coronal plasma leading to condensationins. What distinguishes them is mainly the magnetic field structure. Using MPI-AMRVAC software, we perform multi-dimensional numerical simulations to model coronal rain and prominences in order to understand the physical process of condensation and the dynamics of condensed material in prominences and coronal rain. Additionally, we report on recent development of MPI-AMRVAC 2.0, highlighting its new user-friendly design and new poweful functions.