  We introduce our newly developed two different, three dimensional magneto
hydrodynamical codes in detail. One of our codes is written in the Newtonian
limit (NMHD) and the other is in the fully general relativistic code (GRMHD).
Both codes employ adaptive mesh refinement and, in GRMHD, the metric is evolved
with the "Baumgarte-Shapiro-Shibata-Nakamura" formalism known as the most
stable method at present. We did several test problems and as for the first
practical test, we calculated gravitational collapse of a $15M_\odot$ star.
Main features found from our calculations are; (1) High velocity bipolar
outflow is driven from the proto-neutronstar and moves through along the
rotational axis in strongly magnetized models; (2) A one-armed spiral structure
appears which is originated from the low-$|T/W|$ instability; (3) By comparing
GRMHD and NMHD models, the maximum density increases about $\sim30%$ in GRMHD
models due to the stronger gravitational effect. These features agree very well
with previous studies and our codes are thus reliable to numerical simulation
of gravitational collapse of massive stars.
