  Flares are intense explosions on the solar and stellar surfaces, and solar
flares are sometimes accompanied by filament or prominence eruptions. Recently,
a large filament eruption associated with a superflare on a solar-type star EK
Dra was discovered for the first time. The absorption of the H$\alpha$ spectrum
initially exhibited a blueshift with the velocity of $510$ (km s$^{-1}$), and
decelerated in time probably due to gravity. Stellar coronal mass ejections
(CMEs) were thought to occur, although the filament eruption did not exceed the
escape velocity under the surface gravity. To investigate how such filament
eruption occur and whether CMEs are associated with the filament eruption or
not, we perform one-dimensional hydrodynamic simulation of the flow along an
expanding magnetic loop emulating a filament eruption under adiabatic and
unsteady conditions. The loop configuration and expanding velocity normal to
the loop are specified in the configuration parameters, and we calculate the
line-of-sight velocity of the filament eruption using the velocities along and
normal to the loop. We found that (i) the temporal variations of the H$\alpha$
spectrum for EK Dra can be explained by falling filament eruption in the loop
with longer time and larger spatial scales than that of the Sun, and (ii) the
stellar CMEs are also thought to be associated with the filament eruption from
the superflare on EK Dra, because the rarefied loop unobserved in the H$\alpha$
spectrum needs to expand faster than the escape velocity, whereas the observed
filament eruption does not exceed the escape velocity.
