  1H0323+342 is one of narrow-line radio-loud Seyfert 1 galaxies (RL-NLS1),
which is a new class of gamma-ray emitting AGNs. Narrow-line Seyfert 1 galaxies
(NLS1) have a small-mass black hole, but its mass accretion rate is almost as
high as Eddington limit. Therefore, by observing NLS1s, we can know the
evolution of supermassive black holes at the center of galaxies. Some of NLS1s
are radio-loud and we call them RL-NLS1. From past observations,
multi-wavelength spectrum of RL-NLS1s is similar to that of typical blazars;
the synchrotron emission in the lower energy band up to the optical band, and
inverse Compton scattering of low energy photons from disk, torus, and broad
line region. X-ray band is a transittion region between the synchrotron and
inverse Compton, and also there is a possible disk/corona emission. Therefore,
we studied the energy-dependence of time variability of the X-ray emission of
1H0323+342, which have been observed by Suzaku in 2009 and 2013, in order to
constrain the emission mechanism. We found that the lower energy below 1 keV
and the higher energy above 7 keV show a different variability from the middle
energy band, indicating at least two emission components in the X-ray band.
X-ray spectrum is not a simple power-law, but requires an additional features;
a broken power-law plus flat hard component, or a power-law plus a relativistic
reflection component. Each spectral component seems to vary independently.
