Tracing the evolution of an X-ray selected tidal disruption event

In a program, running since AO7, we have used XMMNewton, Swift, optical andradio observations to monitor the evolution of four tidal disruption eventsdiscovered by a nearreal time comparison of XMM slew data with the ROSATallsky survey. This work has broadly confirmed the original idea that stellardebris returns to the black hole with an index of 5/3 and emits in the softXray band with luminosity following the returning mass. It has shown that thepeak Xray emission is reprocessed and not simply the highenergy tail ofthermal emission. We now wish to investigate questions raised by these detailedobservations: why do few TDE generate a hard Xray component? Why is theemission so volatile in the early phase? Why do Xray selected events not have truncated!, Please see actual data for full text [truncated!, Please see actual data for full text]