  We investigated the effect of magnetic fields on the collision process
between dense molecular cores. We performed three-dimensional
magnetohydrodynamic simulations of collisions between two self-gravitating
cores using the Enzo adaptive mesh refinement code. The core was modeled as a
stable isothermal Bonnor-Ebert (BE) sphere immersed in uniform magnetic fields.
Collisions were characterized by the offset parameter $b$, Mach number of the
initial core $\mathcal{M}$, magnetic field strength $B_{0}$, and angle $\theta$
between the initial magnetic field and collision axis. For head-on ($b = 0$)
collisions, one protostar was formed in the compressed layer. The higher the
magnetic field strength, the lower the accretion rate. For models with $b = 0$
and $\theta = 90^{\circ}$, the accretion rate was more dependent on the initial
magnetic field strength compared with $b = 0$ and $\theta = 0^{\circ}$ models.
For off-center ($b = 1$) collisions, the higher specific angular momentum
increased; therefore, the gas motion was complicated. In models with $b = 1$
and $\mathcal{M} = 1$, the number of protostars and gas motion highly depended
on $B_{0}$ and $\theta$. For models with $b = 1$ and $\mathcal{M} = 3$, no
significant shock-compressed layer was formed and star formation was not
triggered.
