This study presents a multistream superthermal electron transport model for the Mars space environment. This model includes the magnetic inhomogeneity effects, which is vital to understand electron motion around Mars. The convergence tests on the step sizes of variables are carried out and appropriate grid setups are determined. In addition, we have examined three physical parameters, F _10.7 values, thermal electron/plasma density, and neutral densities. Through the investigation of F _10.7 values, an interesting fact about the Hinteregger model is found that the photon flux of each wavelength is scaled differently. The resultant photoelectron fluxes also show a nonuniform percentage of increase. The results of plasma density and neutral densities tests are consistent with previous theories, such as the expected degradation of fluxes in the low‐energy range with increased thermal electron/plasma density, and the elevated peak altitude of photoelectron fluxes with increased neutral densities. The examination of these physical parameters indicates the model's ability to simulate various environments and verifies the model's performance. Finally, a data‐model comparison is carried out and the modeled omnidirectional fluxes agree well (within a factor of 2) with the observation.

Key Points

Presents a time‐dependent, multistream hot electron transport model for Mars Conducted convergence tests of this model for closed magnetic field lines Validated the model's performance by examining several physical parameters