086156

In the young system of WASP-18 the coronal emission is almost two orders of magnitude lower than expected for a star of its spectral type openParF6closePar and age openPar 800 MyrclosePar. The puzzling behavior could be explained as due to tidal interaction with its very massive hot Jupiter openPar10 M J closePar that prevents the formation of a magnetic dynamo in the shallow convective zone of the star and of thus of the corona. Here we want to observe the system of KELT-24 which is very similar to WASP-18. It is formed by an F5 star orbited by a massive hot Jupiter every 5 days. A measurement of its X-ray flux and luminosity derived from a 25 ks XMM-EPIC exposure can tell us if KELT-24 behaves like a young F type star of Hyades or if its X-ray activity is quenched by the interaction with its 5 M_J hot Jupiter.