GASP (GAs Stripping Phenomena in galaxies with MUSE) is a survey of galaxies at z=~0.05 located in different environments, from the field to clusters. The project aims to clarify how, where and why the gas removal occurs. The MUSE observations revealed ram pressure stripped Hαemitting extraplanar tails in most of the stripping cluster candidates. All galaxies present bright Hα clumps in their tails as well as interclump regions of more diffuse emission. Using diagnostic BPT diagrams we conclude that in-situ SF is the dominant gas ionization mechanism in all the tails. I will summarize the main results on the star formation process in the tails, and on how the star formation rate depends on the properties of the galaxy and of its environment; I will also present some of the questions our work has opened and that will be addressed by using the GASP MUSE data and its multiwavelength ongoing follow-ups, including an ongoing observing programme with HST.