The ?radiation inner edge? of an accretion disk is defined as the inner boundary of the region from which most of the luminosity emerges. Similarly, the ?reflection edge? is the smallest radius capable of producing a significant X-ray reflection of the fluorescent iron line. For black hole accretion disks with very sub-Eddington luminosities these and all other ?inner edges? locate at ISCO. Thus, in this case, one may rightly consider ISCO as the unique inner edge of the black hole accretion disk. However, even for moderate luminosities, there is no such unique inner edge as differently defined edges locate at different places. Several of them are significantly closer to the black hole than ISCO. The differences grow with the increasing luminosity. Fornearly Eddington luminosities, they are so huge that the notion of the inner edge losses all practical significance.