  The formation and evolution of spiral arms in low surface brightness galaxies
(LSBs) are not well-understood. We study the dynamics of spiral arms in two
prototypical LSBs, F568-VI and F568-01, using both analytical models and N-body
+ hydrodynamical simulations. We first consider the disk as a 2-component
system of gravitationally-coupled stars and gas in the force field of a
\emph{spherical} dark matter halo, subjected to local, non-axisymmetric
perturbations. However, no local spirals are formed. We next assume the disk to
be a 1-component system of stars in the net gravitational potential of a galaxy
with a \emph{spherical} dark matter halo perturbed by a global $m=2$
instability. In this case, the growth time for spiral formation was low, equal
to 0.78 and 0.96 Gyrs, respectively, corresponding to a few dynamical times of
the galaxies. Finally, we simulate the LSBs using the N-body + hydrodynamical
simulation code RAMSES. \emph{Our results show that a quadrupolar field
associated with an oblate halo with an axial ratio of 0.7} is necessary to
drive a long-lived global spiral in the LSB disks. Further, feedback
corresponding to a supernova mass fraction of $\sim$ 0.05 is essential to
comply with the observed stellar surface density. The simulated spirals
survives for about ten dynamical times and the average pattern speed lies
between 10 - 15 $\rm{kms^{-1}{kpc}^{-1}}$. The spiral arm thus formed is
therefore a transient global pattern driven by the tidal field of the oblate
dark matter halo.
