  We study the EUV/soft X-ray emission generated by charge transfer between
solar wind heavy ions and interstellar H and He neutral atoms in the inner
Heliosphere. We present heliospheric maps and spectra for stationary solar
wind, depending on solar cycle phase, solar wind anisotropies and composition,
line of sight direction and observer position. A time-dependant simulation of
the X-ray intensity variations due to temporary solar wind enhancement is
compared to XMM Newton recorded data of the Hubble Deep Field North observation
(Snowden et al. 2004). Results show that the heliospheric component can explain
a large fraction of the line intensity below 1.3 keV, strongly attenuating the
need for soft X-ray emission from the Local Interstellar Bubble.
