  We run two GRRMHD simulations of super-Eddington accretion disks around a
black hole and a non-magnetized, non-rotating neutron star. The neutron star
was modeled using a reflective inner boundary condition. We observe the
formation of a transition layer in the inner region of the disk in the neutron
star simulation which leads to a larger mass outflow rate and a lower radiative
luminosity over the black hole case. Sphereization of the flow leads to an
observable luminosity at infinity around the Eddington value when viewed from
all directions for the neutron star case, contrasting to the black hole case
where collimation of the emission leads to observable luminosities about an
order of magnitude higher when observed along the disk axis. We find the
outflow to be optically thick to scattering, which would lead to the obscuring
of any neutron star pulsations observed in corresponding ULXs.
