ENA imaging simulation of the distant planetary magnetosphere and ENA emission discussion of the solar wind

Whether the “ENA ribbon” image scanned remotely by IBEX-Hi at the lunar Resonance orbit really comes from the heliopause? It involves assessing the scale of solar wind particle loss throughout the solar system. The ENA imaging simulation results at the Lagrange point show that the scale of the planetary magnetosphere with a telemetry distance of AU magnitude is too small to contribute to “ENA ribbon”. But the simulated effective ENA differential fluxes provide a reference for the physical scale evaluation of the huge magnetic structure in the heliopause. Near earth orbit, the ENA differential flux generated by the charge exchange between solar wind ions and local neutral gas is equivalent to the measurements of “ENA ribbon”, which may be the main ENA emission source of the “ENA ribbon”. If the ion flow of solar wind forms a tailward distribution loop under galactic wind pressure, the morphology difference of the ENA ribbon measured by IBEX-Hi between the Ram and anti-ram direction can be explained. 2D ENA imaging measurements at Lagrange points proposed here can be used to investigate the ENA ribbon origination by using the energy spectral lag vs disparity of ENA images.