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

Aug 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010pasj...62..981e&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.62, No.4, pp.981--986

Astronomy and Astrophysics

Astronomy

6

Earth, Sun: Solar-Terrestrial Relations, Sun: Solar Wind, X-Rays: Diffuse Background

Scientific paper

We report on 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 sr-1) to be emitted inside the heavily obscured galactic disk. It showed a factor of two time variation that showed a significant (˜4σ) correlation with the solar-wind O7+ ion flux. The high line intensity and 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 while considering a line-of-sight direction and also theoretical distribution models of the neutral hydrogen and solar wind around Earth. Our results indicate that X-ray observations of geocoronal solar-wind charge-exchange emission can be used to constrain these models.

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