OVI, NV, and CIV in the galactic halo. I. Velocity-dependent ionization models

We explore theoretical models of the ionization ratios of the Li-like absorbers N V, O VI, and C IV, in the Galactic halo. These ions are believed to form in nonequilibrium processes, such as shocks, evaporative interfaces, or rapidly cooling gas, all of which trace the dynamics of the interstellar medium. As a useful new diagnostic, we focus on velocity-resolved signatures of several common physical structures: ( 1) a cooling Galactic fountain flow that rises, cools, and recombines as it returns to the disk; (2) shocks moving toward the observer; and ( 3) a conductive interface with the observer located in the hotter gas. This last geometry occurs with the solar system inside a hot bubble, or when one looks out through the fragmenting top shell of our local bubble blown into the halo as part of the Galactic fountain. In our second paper, these models are compared to ionization ratio data from Far Ultraviolet Spectroscopic Explorer (FUSE) and Hubble Space Telescope.