  A possible model of twin high-frequency QPOs (HF QPOs) of microquasars is
examined. The disk is assumed to have global magnetic fields and to be deformed
with a two-armed pattern. In this deformed disk, set of a two-armed ($m=2$)
vertical p-mode oscillation and an axisymmetric ($m=0$) g-mode oscillation are
considered. They resonantly interact through the disk deformation when their
frequencies are the same. This resonant interaction amplifies the set of the
above oscillations in the case where these two oscillations have wave energies
of opposite signs. These oscillations are assumed to be excited most
efficiently in the case where the radial group velocities of these two waves
vanish at the same place. The above set of oscillations is not unique,
depending on the node number, $n$, of oscillations in the vertical direction.
We consider that the basic two sets of oscillations correspond to the twin
QPOs. The frequencies of these oscillations depend on disk parameters such as
strength of magnetic fields. For observational mass ranges of GRS 1915+105, GRO
J1655-40, XTE J1550-564, and H1743-322, spins of these sources are estimated.
High spins of these sources can be described if the disks have weak poloidal
magnetic fields as well as toroidal magnetic fields of moderate strength. In
this model the 3 : 2 frequency ratio of high-frequency QPOs is not related to
their excitation, but occurs by chance.
