  A model of geocoronal solar wind charge exchange (SWCX) emission was built
and compared to five Suzaku detections of bright geocoronal SWCX events. An
exospheric neutral hydrogen distribution model, charge exchange cross sections,
solar wind ion data taken with the ACE and WIND satellites, and magnetic field
models of the Earth's magnetosphere are all combined in order to predict
time-variable geocoronal SWCX emission depending on line-of-sight directions of
the Suzaku satellite. The modeled average intensities of O VII emission lines
were consistent with the observed ones within a factor of three in four out of
the five cases except for an event in which a line-of-sight direction was
toward the night side of the high-latitude magnetosheath and a major
geomagnetic storm was observed. Those of O VIII emission lines were
underestimated by a factor of three or more in all the five cases. On the other
hand, the modeled O VII and O VIII light curves reproduced the observed ones
after being scaled by ratios between the observed and modeled average
intensities. In particular, short-term variations due to line-of-sight
directions traversing cusp regions during an orbital motion of the Suzaku
satellite were reproduced. These results are discussed in the context of model
uncertainties.
