Physics‐based formula representations of high‐latitude ionospheric outflows: H⁺ and O⁺ densities, flow velocities, and temperatures versus soft electron precipitation, wave‐driven transverse heating, and solar zenith angle effects

<jats:p>Extensive systematic dynamic fluid kinetic (DyFK) model simulations are conducted to obtain advanced simulation‐based formula representations of ionospheric outflow parameters, for possible use by global magnetospheric modelers. Under F<jats:sub>10.7</jats:sub> levels of 142, corresponding to solar medium conditions, we obtain the H<jats:sup>+</jats:sup> and O<jats:sup>+</jats:sup> outflow densities, flow velocities, and perpendicular and parallel temperatures versus energy fluxes and characteristic energies of soft electron precipitation, wave spectral densities of ion transverse wave heating, and <jats:italic>F</jats:italic> region level solar zenith angle in the high‐latitude auroral region. From the results of hundreds of DyFK simulations of auroral outflows for ranges of each of these driving agents, we depict the H<jats:sup>+</jats:sup> and O<jats:sup>+</jats:sup> outflow density and flow velocity parameters at 3 <jats:italic>R</jats:italic><jats:sub><jats:italic>E</jats:italic></jats:sub> altitude at the ends of these 2‐h simulation runs in spectrogram form versus various pairs of these influencing parameters. We further approximate these results by various distilled formula representations for the O<jats:sup>+</jats:sup> and H<jats:sup>+</jats:sup> outflow velocities, densities, and temperatures at 3 <jats:italic>R</jats:italic><jats:sub><jats:italic>E</jats:italic></jats:sub> altitude, as functions of the above indicated four “driver” parameters. These formula representations provide insight into the physics of these driven outflows, and may provide a convenient set of tools to set the boundary conditions for ionospheric plasma sources in global magnetospheric simulations.</jats:p>