CARBON PLAYS A KEY ROLE IN THE PHYSICAL AND CHEMICAL EVOLUTION OF THE UNIVERSE. CARBON SPECIES ARE IMPORTANT GAS COOLANTS IN BOTH DIFFUSE AND DENSE CLOUDS AND THE MAJORITY OF COMPLEX MOLECULES IN THE INTERSTELLAR MEDIUM (ISM) ARE MADE OF CARBON WITH THE MOST COMPLEX BEING CARBONACEOUS DUST IN THE SOLID STATE. MORE SIGNIFICANTLY CARBON-BASED CHEMISTRY IS CENTRAL TO THE ORIGIN OF LIFE. SOLAR SYSTEM OBJECTS SHOW SYSTEMATIC VARIATIONS IN THEIR CARBON ABUNDANCES CARBON IN COMETS IS SIMILAR TO THAT IN THE ISM WHILE METEORITES ARE DEPLETED IN CARBON (RELATIVE TO SILICON) BY AN ORDER OF MAGNITUDE RELATIVE TO THE SUN AND THE ISM (E.G. PONTOPPIDAN ET AL. 2014). METEORITE AND COMET ANALYSES STUDIES OF CARBON DUST (JONES ET AL. 2016) AND OBSERVATIONS OF YOUNG PROTOPLANETARY DISKS (E.G. BERGIN ET AL. 2016) IMPLY POSSIBLE EVIDENCE FOR CARBON CYCLING FROM THE GAS TO SOLID PHASES IN THE EARLY EVOLUTION OF THE SOLAR NEBULA. HERE WE FOCUS ON THE EVOLUTION OF POLYCYCLIC AROMATIC HYDROCARBONS (PAHS) A UBIQUITOUS COMPONENT OF THE ISM CONSTITUTING 20% OF ALL AVAILABLE CARBON AND ONE OF ITS MOST STABLE FORMS. CARBON IN METEORITES IS MOSTLY IN THE FORM OF ORGANICS (ALEXANDER 2011) INCLUDING AROMATIC MATERIALS SUCH AS SMALL PAHS (C<24) SUGGESTING THE LARGE PAHS (C>30) OF THE ISM COULD SURVIVE AS CONDENSATES IN DISKS AND SERVE AS THE CHEMICAL FEEDSTOCK OF SOLAR SYSTEM ORGANICS. THE RECOGNITION THAT PAHS CONDENSE ONTO ICY GRAINS IN COLD REGIONS UNDER MANY ASTROPHYSICAL SITUATIONS HAS LED TO A SLEW OF EXPERIMENTS STUDYING PAHS IN ICES (E.G. BERNSTEIN ET AL. 1999 GUDIPATI&ALLAMANDOLA 2003 BOUWMAN ET AL. 2011 CUYLLE ET AL. 2014 COOK ET AL. 2015). WATER ICE LOWERS THE IONIZATION POTENTIAL OF PAHS FACILITATING PAH ION FORMATION IN THE PRESENCE OF UV AND PAH DESTRUCTION VIA CHEMICAL DEGRADATION PROCESSES PERHAPS ULTIMATELY LEADING TO THE OBSERVED SOLAR SYSTEM ORGANICS. WE PLAN TO INVESTIGATE THE ROLE OF PAH-WATER ICE CHEMISTRY IN AN EVOLVING NEBULA WITH NEW LABORATORY EXPERIMENTS DESIGNED TO CLOSELY REPLICATE CONDITIONS ACROSS THE ENTIRE PLANET-FORMING ZONE FROM NEAR THE SNOWLINE AT A FEW AU TO COLD REGIONS BEYOND THE KUIPER BELT. THERMOCHEMICAL AND DYNAMICAL DISK MODELS WILL GUIDE EXPERIMENTAL PARAMETERS SUCH AS DENSITIES TEMPERATURES AND STRENGTH OF UV RADIATION FIELDS. FOURIER-TRANSFORM INFRARED (FTIR) AND RAMAN SPECTROSCOPY OF VARIOUS SIZED PAHS (16-50 C ATOMS) ISOLATED IN A WATER ICE MATRIX AND IRRADIATED BY UV PHOTONS WILL DETERMINE BOTH BREAKDOWN (DEGRADATION) RATES AND THE RESULTING PHOTOPRODUCTS; THIS INFORMATION WILL BE ASSIMILATED INTO THE NASA AMES PAH IR SPECTROSCOPIC DATABASE PROVIDING A RICH LEGACY FOR FUTURE WORK ON ORGANICS TO BE PROBED BY SOLAR SYSTEM MISSIONS (E.G. ICY WORLDS MARS 2020) AND TELESCOPE FACILITIES (E.G. JWST). THE PAH DESTRUCTION RATE ON ICES DETERMINED FROM THE EXPERIMENTS WILL BE INCORPORATED INTO DISK EVOLUTION MODELS TO EXAMINE THE POSSIBLE SURVIVAL OF PAHS AS CONDENSATES/COMPLEX ORGANICS ON DISKS AND QUANTIFY THIS MODE OF DELIVERY OF CARBON TO THE INNER DISK.