Suzaku was lunched on July 2005 and completed its scientific observations in June 2015.
It has advantage especially in the Fe K shell band with its low background, large effective area and medium energy resolution,
and hard X-ray above 10 keV with high sensitivity.
In CH Cyg, drastically varying fluorescent Fe K$_\alpha$ line was detected.
The temporal extraordinary large equivalent width of $\sim1.4$ keV
is considered to be caused by scattered X-rays and a occultation of the intrinsic source.
Plasmas in quiescence and outburst of SS Cyg are surrounded by reflectors
with solid angles of $\Omega/(2\pi) = 1.7\pm0.3$ and $0.9^{+0.5}_{-0.4}$, respectively.
The quiescence case is consistent with the traditional boundary layer,
however, the outburst case implies that the plasma locates on the extensive flat reflector.
Non-thermal X-ray was detected from nova for the first time in V2491 Cyg 9 days after the nova event,
whose spectrum can be reproduced by power-law of photon index of $\Gamma = 0.1 \pm 0.2$.
In V1223 Sgr, energy centroid synchronizing with the WD spin was detected in the fluorescent Fe K$_\alpha$ line.
It is suggested to be emitted by the pre-shock accreting matter.
Recently, thermal and reflection X-ray spectral models of the intermediate polar were updated
including variety of the specific accretion rate, dipolar geometry, spherical shape of the reflector and
physical quantities distributions in the accretion flow etc..
The WD masses were estimated at $0.91^{+0.08}_{-0.03}$ $M_{\odot}$ and $0.65^{+0.11}_{-0.12}$ $M_{\odot}$
for V1223 Sgr and EX Hya with application of the new models.
X-ray observatory ASTRO-H will be launched in February 2016.
It will be accomplish energy resolution of $\sim$7 eV at 6 keV with the SXS system,
high sensitivity and large effective area measurement above 10 keV by the HXI system
and large field of view observation (38$\times$38 arcmin$^2$) with the SXI system.
They will enable us to directly diagnose plasma density with the triplet of the He-like ions,
the detailed gaseous dynamics analysis, geometrical inspection and more frequent serendipitous source detection.