Magnetic reconnection is an efficient mechanism by which magnetic energy can be quickly converted into thermal and kinetic energies of plasma in addition to nonthermal energy. As magnetic field exists everywhere in the universe, magnetic reconnection is ubiquitous in various plasmas, including interstellar and intergalactic media, solar and stellar atmospheres, terrestrial magnetosphere, tokamaks, and so on. In this talk, I will first give a brief introduction to the application of magnetic reconnection in various astrophysical processes, and then present the details on how we apply the magnetic reconnection to explain the sophisticated features of solar eruptions, including solar flares, coronal mass ejections, solar coronal bright points.