Abstract
We found the intensity variations of OVII Kα line (0.56 keV) among the multiple observations of two blank sky fields toward NGC2992 and MBM16 with Suzaku. The OVII enhancement in the same line of sight are thought to be related to the Solar Wind Charge Exchange (SWCX) induced emission in the Helium Focusing Cone, depending the different observer's site by the yearly revolution around the Sun. We also simulated the SWCX induced OVII intensities reacted with the neutrals in the Heliosphere including the He Cone. The simulated OVII intensities were comparable to the observed intensity for MBM16 (dense molecular cloud within Local Hot Bubble), while the simulation amounted to about half of the observation for NGC2992. The origin of the half of observed OVII toward NGC2992 is thought to the distant hot plasma of our Galaxy.
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