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Energetic neutral atom (ENA) models typically require post-processingroutines to convert the distributions of plasma and H atoms into ENA maps. Herewe investigate how two different kinetic-MHD models of the heliosphere (the BUand Moscow models) manifest in modeled ENA maps using the same prescription andhow they compare with Interstellar Boundary Explorer (IBEX) observations. BothMHD models treat the solar wind as a single-ion plasma for protons, whichinclude thermal solar wind ions, pick-up ions (PUIs), and electrons. Our ENAprescription partitions the plasma into three distinct ion populations (thermalsolar wind, PUIs transmitted and ones energized at the termination shock) andmodels the populations with Maxwellian distributions. Both kinetic-MHDheliospheric models produce a heliotail with heliosheath plasma organized bythe solar magnetic field into two distinct north and south columns that becomelobes of high mass flux flowing down the heliotail, though in the BU model theISM flows between the two lobes at distances in the heliotail larger than 300AU. While our prescription produces similar ENA maps for the two differentplasma and H atom solutions at the IBEX-Hi energy range (0.5 - 6 keV), themodeled ENA maps require a scaling factor of ~2 to be in agreement with thedata. This problem is present in other ENA models with the Maxwellianapproximation of multiple ion species and indicates that a higher neutraldensity or some acceleration of PUIs in the heliosheath is required.

astrophysical journal/the astrophysical journal

Signature of a heliotail organized by the solar magnetic field and the  role of non-ideal processes in modeled IBEX ENA maps: a comparison of the BU  and Moscow MHD models