The question of how many satellites it would take to accurately map the spatial distribution of ionospheric outflow is addressed in this study. Given an outflow spatial map, this image is then reconstructed from a limited number virtual satellite pass extractions from the original values. An assessment is conducted of the goodness of fit as a function of number of satellites in the reconstruction, placement of the satellite trajectories relative to the polar cap and auroral oval, season and universal time (i.e., dipole tilt relative to the Sun), geomagnetic activity level, and interpolation technique. It is found that the accuracy of the reconstructions increases sharply from one to a few satellites, but then improves only marginally with additional spacecraft beyond ~4. Increased dwell time of the satellite trajectories in the auroral zone improves the reconstruction, therefore a high-but-not-exactly-polar orbit is most effective for this task. Local time coverage is also an important factor, shifting the auroral zone to different locations relative to the virtual satellite orbit paths. The expansion and contraction of the polar cap and auroral zone with geomagnetic activity influences the coverage of the key outflow regions, with different optimal orbit configurations for each level of activity. Finally, it is found that reconstructing each magnetic latitude band individually produces a better fit to the original image than 2-D image reconstruction method (e.g., triangulation). A high-latitude, high-altitude constellation mission concept is presented that achieves acceptably accurate outflow reconstructions.

Ionospheric conductance plays a crucial and active role in magnetosphere-ionosphere-thermosphere coupling processes. Despite its importance, direct global observations of conductance are unavailable. This limitation inspires the development of empirical models that are widely used to specify global distributions of conductance indirectly. In this work, a new model (COMPASS) describing the statistical relationships between conductance and Field-Aligned Currents (FACs) is presented. The conductance was determined by the electron densities measured by Poker Flat Incoherent Scattering Radar (PFISR), and the FACs were determined by the magnetic perturbations measured by SWARM. Between 2014 and 2020, there were $\sim$3900 conjunction events between PFISR and SWARM, providing a large dataset for investigating the relationship between conductance and FACs. It is found that both Hall and Pedersen conductances vary as a power of $|j_{\parallel}|$, and the power index $a$ is between 0 and 0.5. This power index $a$ depends on the Magnetic Local Time (MLT) and the direction of FACs: (1) The largest power index is obtained on the dawn side, and the minimum is at noon, suggesting the strongest/weakest correlation in the dawn/noon sector; (2) the power indices are positive for both upward and downward FACs and are larger for upward FACs than downward FACs, except in the dusk sector. The underlying physical mechanisms of the observed variations of the model parameters are also discussed. This work sheds light on the complicated relationship between FACs and conductance and provides a convenient way to specify global distributions of the auroral zone conductance.