  Here we extend the exploration of significantly super-Chandrasekhar
magnetised white dwarfs by numerically computing axisymmetric stationary
equilibria of differentially rotating magnetised polytropic compact stars in
general relativity (GR), within the ideal magnetohydrodynamic regime. We use a
general relativistic magnetohydrodynamic (GRMHD) framework that describes
rotating and magnetised axisymmetric white dwarfs, choosing appropriate
rotation laws and magnetic field profiles (toroidal and poloidal). The
numerical procedure for finding solutions in this framework uses the 3+1
formalism of numerical relativity, implemented in the open source XNS code. We
construct equilibrium sequences by varying different physical quantities in
turn, and highlight the plausible existence of super-Chandrasekhar white
dwarfs, with masses in the range of 2-3 solar mass, with central (deep
interior) magnetic fields of the order of $10^{14}$ Gauss and differential
rotation with surface time periods of about 1-10 seconds. We note that such
white dwarfs are candidates for the progenitors of peculiar, overluminous type
Ia supernovae, to which observational evidence ascribes mass in the range
2.1-2.8 solar mass. We also present some interesting results related to the
structure of such white dwarfs, especially the existence of polar hollows in
special cases.
