  We investigate the occurrence of rapid-rotation induced chemically
homogeneous evolution (CHE) due to strong tides and mass accretion in binaries.
To this end, we generalize the relation in Packet (1981) to calculate the
minimum angular momentum (AM) accretion required by a secondary star to
experience accretion-induced CHE. Contrary to traditionally assumed 5-10
percent accretion of initial mass ($Z \lesssim 0.004$, $M \gtrsim$ 20
M$_{\odot}$) for spinning up the accretor (resulting in CHE) this value can
drop to $\sim$ 2 percent for efficient AM accretion while for certain systems
it could be substantially larger. We conduct a population study using
\textsc{bpass} by evolving stars under the influence of strong tides in
short-period binaries and also account for the updated effect of
accretion-induced spin-up. We find accretion CHE (compared to tidal CHE) to be
the dominant means of producing homogeneous stars even at 10 percent AM
accretion efficiency during mass transfer. Unlike tidal CHE, it is seen that CH
stars arising due to accretion can retain a larger fraction of their AM till
core collapse. Thus we show that accretion CHE could be an important formation
channel for energetic electromagnetic transients like GRBs, Ic-BL (SLSN-I,
Ic-BL) under the collapsar (magnetar) formalism and a single CH star could lead
to both the transients under their respective formation scenario. Lastly, we
show that under the current treatment of CHE, the emission rate of ionizing
photons by such stars decreases more rapidly at higher metallicities than
previously predicted.
