Magnetic reconnection is thought to happen in the ubiquitous magnetic fields of the Sun and it is generally accepted that reconnection plays an important role in most of the solar activity phenomena. However, to prove this is not trivial, since we can not "see" reconnection happening. On the other hand, from multi-wavelength observations and their combination with modelling we can provide evidence for the existence of many of the theoretically expected consequences of reconnection. We do have mounting circumstantial evidence that reconnection is indeed at work in e.g. jets, flares, CMEs. Such observations, in turn, introduce constraints that help to drive and improve the models. I summarize some key observations that have helped to support the case for reconnection while improving our understanding of the behaviour of solar atmospheric plasmas and magnetic fields.
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