  A new rotating generalization of the Damour-Solodukhin wormhole (RDSWH),
called Kerr-like wormhole, has recently been proposed and investigated by Bueno
\textit{et al} for echoes in the gravitational wave signal. We show a novel
feature of the RDSWH, viz., that the kinematic properties such as the ISCO\ or
marginally stable radius $r_{\text{ms}}$, efficiency $\epsilon$ and the disk
potential $V_{\text{eff}}$ are \textit{independent} of $\lambda$ (which means
they are identical to their KBH counterparts for any given spin). Differences
however appear in the emissivity properties for higher values $0.1<\lambda\leq
1$ (say) and for the extreme spin $a_{\star}=0.998$. The kinematic and
emissivity are generic properties as variations of the wormhole mass and the
rate of accretion within the model preserve these properties. Specifically, the
behavior of the luminosity peak is quite opposite to each other for the two
objects, which could be useful from the viewpoint of observations. Apart from
this, an estimate of the difference $\Delta_{\lambda}$ in the maxima of flux of
radiation $F(r)$ shows non-zero values but is too tiny to be observable at
present for $\lambda < 10^{-3}$ permitted by the strong lensing bound. The
broad conclusion is that RDSWH\ are experimentally indistinguishable from KBH
by accretion characteristics.
