Coronal holes and active regions are typical magnetic structures found in the solar atmosphere. In the present work we propose several magnetohydrostatic equilibrium solutions representative of these structures in two-dimensions. Our models include the effect of a finite plasma-β and gravity but the distinctive feature is the incorporation of a thermal structure with properties akin to those reported by the observations. We have developed a semi-analytical method to compute the equilibrium configuration. Using this method we obtain cold an underdense plasma structures in open magnetic fields representing coronal holes, while in closed magnetic configurations we achieve the characteristic hot and overdense plasma arrangements of active regions. Although coronal holes and active regions seem to be antagonistic structures, we find that they can be described using a common thermal structure that depends on the flux function. Apart from the force balance, the energy balance is included in the constructed models using an “a posteriori” approach. From the two-dimensional computation of thermal conduction and radiative losses in our models we infer the required heating function to achieve energy equilibrium. We find that the temperature dependence with height is an important parameter that may prevent the system to accomplish thermal balance at certain spatial locations. The implications of these results are discussed in detail.