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Black holes depend only on mass and spin, while what we see from theaccretion flow in steady state depends also on mass accretion rate and (weakly)inclination. Hence we should be able to scale the accretion flow propertiesfrom the stellar to the supermassive black holes. But the data show significantdifferences between these two types of systems, suggesting that we are missingsome crucial physics in AGN. One of these differences is the soft X-ray excesswhich is seen ubiquitously in bright AGN, but only occasionally in BHB. Anotheris the much faster variability seen in the high energy tail of high massaccretion rate AGN compared to that seen in the tail of BHB. We show that whilethis variability is not understood, it can be used via the new spectral-timingtechniques to constrain the nature of the soft X-ray excess. The coherence,lag-frequency and lag-energy results strongly support this being an additionallow temperature Comptonisation component rather than extreme relativisticallysmeared reflection in the 'simple' Narrow Line Seyfert 1 PG1244+026.

Scaling accretion flow models from BHB to AGN - Why doesn't it work?