Solar flares are powerful radiations occuring in the Suns atmosphere. They are powered by magnetic reconnection, a phemonenon that can convert magnetic energy into other forms of energy such as heat and kinetic energy, and it is believed to be ubiquitous in the universe. With the ever increasing spatial and temporal resolutions of solar observations, as well as numerical simulations benefiting from increasing computer power, we can now probe into the nature and the characteristics of magnetic reconnection in 3D to better understand its consequences during eruptive flares in our stars atmosphere. We review in the following the efforts made on different fronts to approach the problem of magnetic reconnection. In particular, we will see how understanding the magnetic topology in 3D helps locating the most probable regions for reconnection to occur, how the current layer evolves in 3D and how reconnection leads to the formation of flux ropes, plasmoids and flaring loops.
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