Right: Ratio ﹩\Gamma =I_{\mathrm{O}\,\,{}^{{\rm{\small VI}}}\,\lambda 1032}/ I_{\mathrm{O}\,\,{}^{{\rm{\small VI}}}\,\lambda 1037}﹩, synthesized from our model 1, assuming that the oxygen abundance in the streamer closed region is depleted by a factor of 1/100. Higher values of the ratio are brighter and lower values are darker, with contour plots (thick lines) of values ﹩\Gamma =﹩ 0.25, 1.0, 2.0, 2.5, 3.0, and 3.5. Left: Outflow ﹩\mathrm{O}\,^{5+}﹩ velocity V_O in km s⁻¹. Regions where ﹩\Gamma < 2﹩ surround the outflow velocity contour ﹩V_{\mathrm{O}\,}\sim 175﹩ km s⁻¹ (indicated as a contour plot in the right panel), for which the C II λ1037.02 line pumping effect on the O VI λ1037 line is maximized. This region extends up to the region where velocities reach ~380 km s⁻¹, for which the pumping by the C II λ1036.34 line is maximized. Thin white lines are selected magnetic field lines in the plane of the sky.