  We present a model of the analog geometry in a magnetohydrodynamic (MHD)
flow. For the MHD flow with magnetic pressure-dominated and gas
pressure-dominated conditions, we obtain the magnetoacoustic metric for the
fast MHD mode. For the slow MHD mode, on the other hand, the wave is governed
by the advective-type equation without an isotropic dispersion term. Thus, the
"distance" perpendicular to the wave propagation is not defined and the
magnetoacoustic metric cannot be introduced. To investigate the properties of
the magnetoacoustic geometry for the fast mode, we prepare a two-dimensional
axisymmetric inflow and examine the behavior of magnetoacoustic rays which is a
counterpart of the MHD waves in the eikonal limit. We find that the
magnetoacoustic geometry is classified into three types depending on two
parameters characterizing the background flow:~analog spacetimes of rotating
black holes, ultra spinning stars with ergoregions, and spinning stars without
ergoregions. We address the effects of the magnetic pressure on the effective
geometries.
