ASTRONOMICAL OBSERVATIONS IN THE MID/FAR-INFRARED WAVELENGTHS CONTINUE TO ADVANCE OUR UNDERSTANDING OF THE EVOLUTION OF STARS AND GALAXIES. THE FINE STRUCTURE EMISSION LINES IN THE MID/FAR-INFRARED WAVELENGTHS ARISING FROM FOR EXAMPLE HIGHLY-CHARGED ATOMIC IONS (MID-IR) AND OXYGEN ATOMS (FAR-IR) ARE IMPORTANT TARGETS OF OBSERVATIONS WITH THE NASA ASTROPHYSICS MISSIONS JWST AND/OR SOFIA AS WELL AS THE ARCHIVAL PAST MISSIONS HERSCHEL SPITZER AND THE INFRARED SPACE OBSERVATORY (ISO). IN THE CASE OF IONS BECAUSE THEY ARE CREATED BY HIGH ENERGY PHENOMENA ORIGINATING IN CORES AND SHOCKS OF ASTRONOMICAL OBJECTS THEIR FINE STRUCTURE LINES BRIDGE DATA FROM THESE MISSIONS TO DATA FROM FOR EXAMPLE CHANDRA AS WELL AS TO OPTICAL DATA FROM HST. THE FINE STRUCTURE EMISSION LINES ARE HIGHLY VALUED DIAGNOSTICS OF ENERGIES AND DENSITIES IN GALAXIES PLANETARY NEBULAE AND STARS AND AS PROBES OF WARM GASES IN CIRCUMSTELLAR DISKS AND OUTFLOWS. DIAGNOSTIC VALUES OF THE FINE STRUCTURE EMISSION LINES DEPEND ON THE IONIZATION POTENTIALS OF THE IONS AS WELL AS THEIR FINE STRUCTURE TRANSITIONS (LEADING TO EMISSION LINES) IN RESPONSE TO COLLISIONS WITH ELECTRONS HYDROGEN ATOMS AND OTHER SPECIES. WE WILL PROVIDE RELIABLE CALCULATIONS OF FINE STRUCTURE CHANGING COLLISIONS OF [O I] AND H [NE II] AND H AND [NE III] AND H USING A FULLY QUANTUM-MECHANICAL SCATTERING APPROACH. THE ASSOCIATED EXCITATION AND COOLING RATE COEFFICIENTS WILL BE APPLICABLE TO MODELING OF ASTROPHYSICAL PHENOMENA OBSERVED USING MID/FAR-INFRARED ASTRONOMICAL SPECTROSCOPY AND TRACED THROUGH GAS AROUND ACTIVE GALACTIC NUCLEI AND IRRADIATED PROTOPLANETARY DISKS WITH PARTICULAR RELEVANCE TO JWST/MIRI INCLUDING SEVERAL EARLY RELEASE SCIENCE PROJECTS. THE DATA WILL LEAD TO BETTER MODELS OF IONIC FINE STRUCTURE LINES AS DIAGNOSTICS OF ASTROPHYSICAL ENVIRONMENTS USING SPECTROSCOPIC OBSERVATIONS FROM AIR- AND SPACE-BORNE MISSIONS IN THE MID- AND FAR-INFRARED WAVELENGTHS.