  We examined soft X-ray emission by the solar wind charge-exchange process
around the Earth's magnetosphere using a global magnetohydrodynamic simulation
model. The dayside magnetopause reconnection heats and accelerates the plasma
whereby the X-ray emission becomes as bright as $\sim 6 \times 10^{-6} {\rm\
eV}\ {\rm cm}^{-3}\ {\rm s}^{-1}$ under the southward interplanetary magnetic
field conditions. In particular, under low plasma-$\beta$ solar wind
conditions, we found that the X-ray intensity reflects the bulk motion of
outflows from the reconnection region. We propose that this particular solar
wind condition would allow visualization of the mesoscale magnetopause
reconnection site, as observed in the solar corona.
