We study the X-ray emission of baryon fluid in the universe using the WIGEON cosmological hydrodynamic simulations. It has been revealed that cosmic baryon fluid in the nonlinear regime behaves like Burgers turbulence, i.e. the fluid field consists of shocks. Like turbulence in incompressible fluid, the Burgers turbulence plays an important role in converting the kinetic energy of the fluid to thermal energy and heats the gas. We show that the simulation sample of the CDM model without adding extra heating sources can fit well the observed distributions of X-ray luminosity versus temperature (Lx vs. T) of galaxy groups and is also consistent with the distributions of X-ray luminosity versus velocity dispersion (Lx vs. σ). Because the baryonic gas is multiphase, the Lx−T and Lx−σ distributions are significantly scattered. If we describe the relationships by power laws Lx ∝ T LT and Lx ∝ σLV, we find αLT>2.5 and αLV>2.1. The X-ray background in the soft 0.5−2 keV band emitted by the baryonic gas in the temperature range 105<T<107K has also been calculated. We show that of the total background, (1) no more than 2% comes from the region with temperature less than 106.5 K, and (2) no more than 7% is from the region of dark matter with mass density ρdm<50 ρdm. The region of ρdm>50 ρdm is generally clustered and discretely distributed. Therefore, almost all of the soft X-ray background comes from clustered sources, and the contribution from truly diffuse gas is probably negligible. This point agrees with current X-ray observations.