We briefly discuss the different types of accretion disk models which may be relevant to SS 433, especially in terms of their relation to the regions emitting the strongly red and blue shifted Hα and Hβ lines so peculiarly characteristic of this object. In particular we outline in some detail a subcritical accretion disk associated with the lasing recombination ring model of Ruffini, Fang Li Zhi and their co-workers and describe in a very qualitative way the various thick supercritical disks which may be connected with the formation of relativistic jets in SS 433.