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tokens: X-ray emitting corona. The energetic contribution to the SED of the former is observed to increase over the latter with increasing ṁ ( Vasudevan Fabian 2009 ; Jin et al. 2012 ). This is explained with the increased inner radial extent of the UV disk, at the expenses of the X-ray corona, at larger ṁ compared with lower ṁ . Assuming a constant radiative efficiency above ṁ ∼ 0.01, the relative UV/X-ray flux ratio will thus increase with increasing ṁ , moving from low-luminosity Seyfert galaxies toward higher luminosity-Seyfert galaxies and QSOs. A consequence of our scenario is therefore that the X-ray coronae in Seyfert galaxies will be extended up to a few tens R g , different than in QSOs where they will be very compact, only a few R g in size. Recent observations of distant microlensed QSOs revealed very compact X-ray coronae only ≲10 R g in size ( Chartas et al. 2009c ; Dai et al. 2010 ; MacLeod et al. 2015 ). In comparison, deep and broadband X-ray spectroscopic observations of the local Seyfert Ark 120 suggest an extended corona (∼10 − 40 R g , Matt et al. 2014 ), and a decrease of the corona size with increasing flux of the continuum source ( Porquet et al. 2019 ). Studies of larger samples of sources are clearly needed in order to assess the presence of a statistical difference in X-ray coronal size between Seyfert galaxies and QSOs. Radiation-driven disk winds driven by pressure on spectral lines are a physical component that can explain many observational features of AGN, but not all of them: for example, the BALs observed in the FR I radio galaxies ( Fanaroff Riley 1974 ), which are accreting at low ṁ , must be driven by magnetic pressure. In our scenario, the low and very low ṁ AGN appear as radio loud because they lack strong optical and UV emission, and would correspond to the FR I, or LEG (low excitation galaxies, Laing et al. 1994 ). At higher ṁ , radio-loud AGN appear as FR II (or HEG, high excitation galaxies) and do have an accretion disk (e.g., Ghisellini Celotti 2001 ; Grandi Palumbo 2004 ). The radio loudness associated to their powerful radio jets is probably driven by the efficient extraction of rotational energy from both the disk ( Blandford Payne 1982 ) and the black hole ( Blandford Znajek 1977 ); however, the exact physical mechanism behind the launching and acceleration of the most powerful radio jets is still under investigation (see Czerny You 2016 , for a recent review). We note how there are no apparent differences in observed properties such as black hole mass, Eddington ratio, and BLR size between radio-loud and radio-quiet BAL QSOs ( Bruni et al. 2014 ), suggesting that the physical difference between them might reside in different black hole spin values. The scarcity of powerful radio-loud FR II BAL QSOs is probably due to the combination of a large black hole mass needed to have a RL AGN ( Laor 2000 ), which is possibly related to the merger history of the host galaxies, where coherent mergers can increase