  Coronal mass ejections (CMEs) on stars can change the stars' magnetic field
configurations and mass loss rates during the eruption and propagation and
therefore, may affect the stars' rotation properties on long time-scales. The
dynamics of stellar CMEs and their influence on the stellar angular momentum
loss rate are not yet well understood. In order to start investigating these
CME-related aspects on other stars, we conducted a series of
magnetohydrodynamic simulations of CMEs on a solar-type star of moderate
activity levels. The propagation and evolution of the CMEs were traced in the
three-dimensional outputs and the temporal evolution of their dynamic
properties (such as masses, velocities, and kinetic energies) were determined.
The simulated stellar CMEs are more massive and energetic than their solar
analog, which is a result of the stronger magnetic field on the surface of the
simulated star than that of the Sun. The simulated CMEs display masses ranging
from ~10^16 g to ~10^18 g and kinetic energies from ~10^31 erg to ~10^33 erg.
We also investigated the instantaneous influence of the CMEs to the star's
angular momentum loss rate. Our results suggest that angular momentum can
either be added to or be removed from the star during the evolution of CME
events. We found a positive correlation between the amplitude of the angular
momentum loss rate variation and the CME's kinetic energy as well as mass,
suggesting that more energetic/massive CMEs have higher possibility to add
angular momentum to the star.
