  The masses and radii of non-rotating and rotating configurations of pure
hadronic stars mixed with self-interacting fermionic Asymmetric Dark Matter are
calculated within the two-fluid formalism of stellar structure equations in
general relativity. The Equation of State (EoS) of nuclear matter is obtained
from the density dependent M3Y effective nucleon-nucleon interaction. We
consider dark matter particle mass of 1 GeV. The EoS of self-interacting dark
matter is taken from two-body repulsive interactions of the scale of strong
interactions. We explore the conditions of equal and different rotational
frequencies of nuclear matter and dark matter and find that the maximum mass of
differentially rotating stars with self-interacting dark matter to be $\sim
1.94 M_\odot$ with radius $\sim 10.4$ kms.
