the disc primarily through the rotation of the central object and pointed out that different conclusions might therefore be reached with different disc models.

Since the black holes supposed in astrophysical sources may be spinning rapidly, the question also appeared naturally whether the rotating (Kerr) space-time geometry could not itself accelerate and/or axially (pre-)collimate outflows emerging from its inner region — see [@BicakSH-93], [@deFeliceZ-00], [@Williams-04], [@TakamiK-09], [@GarielMMS-10] and [@deFreitasPachecoGM-12]. However, today the astrophysical jets are believed to be mainly driven by magneto-hydrodynamical effects (e.g. @PudritzHG-12).

In the meantime, the interest in [*radiation*]{} acceleration of jets has continued and more astrophysically quite sophisticated treatments have appeared since then, incorporating radiation from specific models of accretion discs, a more realistic description of the radiation-particle interaction (dependent on energy and taking into account heating of the particle as well as its radiation losses), specific particle content of the outflow (electron-proton or/and electron-positron jets, for example), magnetic fields or/and special geometry of the interaction region (“funnels" of thick accretion discs, in particular) — see [@SikoraSBM-96], [@InoueT-97], [@MadauT-00], [@ChattopadhyayCh-02], [@OriharaF-03], [@FukueA-06], [@TakeuchiOM-10], [@KumarChM-14], [@Cao-14] and their references. Let us conclude this overview by [@KoutsantoniouC-14] who have studied the influence of disc radiation on dynamics of 