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

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

2010-06-28

arxiv.org/abs/1006.5253v1

Astronomy and Astrophysics

Astrophysics

Earth and Planetary Astrophysics

14 pages, 5 figures; accepted to PASJ

Scientific paper

We report the detection of a time variable OVII line emission in a deep 100 ks Suzaku X-ray Imaging Spectrometer spectrum of the Galactic Ridge X-ray emission. The observed line intensity is too strong (11+/-2 line unit or photon cm^-2 s^-1 str^-1) to be emitted inside the heavily obscured Galactic disk. It showed 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 the good time correlation with the solar wind strongly suggests that it originated from geocoronal solar wind charge exchange emission. We discuss the X-ray line intensity considering a line of sight direction and also theoretical distribution models of the neutral hydrogen and solar wind around the Earth. Our results indicate that X-ray observationsof geocoronal solar wind charge exchange emission can be used to constrain these models.

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