Disruption of coronal activity due to a massive hot Jupiter.

In the young system of WASP18 the coronal emission is almost two orders ofmagnitude lower than expected for a star of its spectral type (F6) and age ( 800Myr). The puzzling behavior could be explained as due to tidal interaction withits very massive hot Jupiter (10 M J ) that prevents the formation of a magneticdynamo in the shallow convective zone of the star and of thus of the corona.Here we want to observe the system of KELT24 which is very similar to WASP18.It is formed by an F5 star orbited by a massive hot Jupiter every 5 days. Ameasurement of its Xray flux and luminosity derived from a 25 ks XMMEPICexposure can tell us if KELT24 behaves like a young F type star of Hyades or ifits Xray activity is quenched by the interaction with its 5 M_J hot Jupiter. truncated!, Please see actual data for full text [truncated!, Please see actual data for full text]