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We report the detection of a time variable OVII line emission in a deep 100ks Suzaku X-ray Imaging Spectrometer spectrum of the Galactic Ridge X-rayemission. The observed line intensity is too strong (11+/-2 line unit or photoncm^-2 s^-1 str^-1) to be emitted inside the heavily obscured Galactic disk. Itshowed a factor of two time variation which shows a significant (~4 sigma)correlation with the solar wind O^7+ ion flux. The high line intensity and thegood time correlation with the solar wind strongly suggests that it originatedfrom geocoronal solar wind charge exchange emission. We discuss the X-ray lineintensity considering a line of sight direction and also theoreticaldistribution models of the neutral hydrogen and solar wind around the Earth.Our results indicate that X-ray observationsof geocoronal solar wind chargeexchange emission can be used to constrain these models.

Time Variability of the Geocoronal Solar Wind Charge Exchange in the Direction of the Celestial Equator