Not listed INTERACTING SUPERNOVAE ARE POORLY-UNDERSTOOD ASTRONOMICAL EVENTS WITH GREAT POTENTIAL FOR EXPANDING OUR UNDERSTANDING OF HOW STARS EVOLVE AND DIE AND COULD PROVIDE IMPORTANT CLUES ABOUT THE EARLY FORMATION OF LARGE-SCALE STRUCTURES SUCH AS GALAXIES IN THE UNIVERSE. INTERACTING SUPERNOVAE OCCUR WHEN A STAR EXPLODES WITHIN A DENSE CLOUD OF MATERIAL SHED FROM THE STAR IN THE COURSE OF ITS EVOLUTION. THE RESULTING VIOLENT INTERACTION BETWEEN THE EXPANDING SUPERNOVA EXPLOSION AND THE CLOUD OF CIRCUMSTELLAR MATERIAL CAN LEAD TO AN ENORMOUSLY BRIGHT VISUAL DISPLAY --- INDEED MANY OF THE BRIGHTEST SUPERNOVAE EVER RECORDED ARE THOUGHT TO ARISE FROM CIRCUMSTELLAR INTERACTION. IN ORDER TO UNDERSTAND THE PROPERTIES OF THE PROGENITOR STAR AND THE DETAILS OF THE CIRCUMSTELLAR INTERACTION THERE IS A NEED FOR THEORETICAL MODELS OF INTERACTING SUPERNOVAE. THESE SIMULATED COMPUTER SPECTRA CAN BE DIRECTLY COMPARED TO THE SPECTRA OBSERVED BY TELESCOPES. THESE MODELS ALLOW US TO PROBE THE PHYSICAL CIRCUMSTANCES WHICH UNDERLIE THE OBSERVATIONS. THE SPECTRA OF INTERACTING SUPERNOVAE ARE DOMINATED BY STRONG NARROW EMISSION LINES OF LIGHT ELEMENTS SUCH AS HYDROGEN AND HELIUM. THESE NARROW LINES GIVE TYPE IIN SUPERNOVAE THEIR DESIGNATION. SIMILARLY OBJECTS OF TYPE IAN IBN ICN AND IIN ARE SOMEWHAT DISTINCT BUT ARE ALL DEFINED BY THE NARROW EMISSION LINES THAT RESULT FROM THE INTERACTION OF THEIR EXPANDING ENVELOPES WITH THEIR SURROUNDINGS. THE PHOTOSPHERE IN THESE SUPERNOVAE IS FORMED IN THE MATERIAL ACCRETED DURING THE COASTING PHASE AND MOST OF THE LUMINOSITY HAS ITS ORIGIN FROM THE CONVERSION OF KINETIC EXPLOSION ENERGY INTO LUMINOSITY. BOTH THERMONUCLEAR TYPE IA AND CORE-COLLAPSE TYPES IB/IC AND II SUPERNOVAE MAY BE THE INNER ENGINE. IN FACT SEVERAL TYPE IIN SUPERNOVAE AT EARLY TIMES HAVE LATER BEEN CLASSIFIED AS TYPE IA TYPE IB/C OR TYPE II AS THEIR SPECTRA REVEAL MORE DETAILS ABOUT THE NATURE OF THE CENTRAL EXPLOSION. AS A RESULT OF THE DOMINANCE OF THE INTERACTION MODELS OF INTERACTING SUPERNOVAE MUST TAKE INTO ACCOUNT DESCRIPTIONS OF THE HYDRODYNAMICAL IONIZATION AND LIGHT FRONTS: A FULL RADIATIONHYDRODYNAMICAL PROBLEM. THE LOW DENSITIES IMPLY STRONG DEPARTURES FROM THERMODYNAMIC EQUILIBRIUM AND THUS DEMAND A NON-LTE TREATMENT IN THE RADIATIVE TRANSFER CALCULATION. WE PROPOSE A COLLABORATION BETWEEN THE UNIVERSITY OF OKLAHOMA (OU) AND FLORIDA STATE UNIVERSITY (FSU) TO CALCULATE HYDRODYNAMICAL MODELS LIGHT CURVES AND NLTE SPECTRA OF CIRCUMSTELLAR INTERACTING SUPERNOVAE. WE WILL PARAMETERIZE THE EXPLOSION OF A MASSIVE STAR STUDY THE HYDRODYNAMICAL IMPACT ONTO A CIRCUMSTELLAR MEDIUM AND CALCULATE LIGHT CURVES AND SPECTRA. DIRECT COMPARISON WITH OBSERVED SUPERNOVAE WITH GIVE US DETAILED INFORMATION ON THE PROGENITOR STAR ITS MASS LOSS HISTORY AND THE NATURE OF BINARY STELLAR EVOLUTION. WE WILL CALCULATE EXPLOSION MODELS FOR SOME OF THE STELLARSTRUCTURES AND THE ONGOING INTERACTION WITH THE CIRCUMSTELLAR MATERIAL USING OUR RADIATION HYDRO CODE HYDRA AND NLTE GENERALIZED MODEL ATMOSPHERES CODE PHOENIX. WE INTEND TO FOCUS ON THE PHYSICS OF INTERACTING SUPERNOVAE GOING BEYOND THE REGIME WHERE SELFSIMILAR SOLUTIONS AND PHENOMENOLOGICAL APPROACHES ARE VALID. THIS WILL LIMIT THE PARAMETER SPACE THAT NEEDS TO BE EXAMINED WHILE STILL ALLOWING FOR DIRECT COMPARISON WITH OBSERVATIONS. SINCE MANY INTERACTING SUPERNOVAE ARE EXTREMELY BRIGHT THEY CAN BE SEEN AT THE HIGHEST REDSHIFTS AND ARE GOOD PROBES OF THE DARKAGES. THESE SUPERNOVAE WILL BE WELL OBSERVED BY UPCOMING NASA MISSION JWST AS WELL AS GROUND BASED SURVEYS SUCH AS LSST. THE TOOLS FOR THIS WORK ARE IN PLACE: FSU PI PETER HOEFLICH HAS BEEN DEVELOPING AND USING THE HYDRODYNAMIC CODE HYDRA FOR OVER TWO DECADES AND PI EDDIE BARON (OU) HAS BEEN DEVELOPING THE GENERALIZED STELLAR ATMOSPHERE CODE PHOENIX OVER THE SAME TIME PERIOD. BARON AND HOEFLICH HAVE A GOOD WORKING RELATIONSHIP AND HAVE CROSS COMPARED OUR CODES. ($161) 10/19/20 4 INTERACTING SUPERNOVAE ARE POORLY-UNDERSTOOD ASTRONOMICAL EVENTS WITH GREAT POTENTIAL FOR EXPANDING OUR UNDERSTANDING OF HOW STARS EVOLVE AND DIE, AND COULD PROVIDE IMPORTANT CLUES ABOUT THE EARLY FORMATION OF LARGE- SCALE STRUCTURES SUCH AS GALAXIES IN THE UNIVERSE. INTERACTING SUPERNOVAE OCCUR WHEN A STAR EXPLODES WITHIN A DENSE CLOUD OF MATERIAL SHED FROM THE STAR IN THE COURSE OF ITS EVOLUTION. THE RESULTING VIOLENT INTERACTION BETWEEN THE EXPANDING SUPERNOVA EXPLOSION AND THE CLOUD OF CIRCUMSTELLAR MATERIAL CAN LEAD TO AN ENORMOUSLY BRIGHT VISUAL DISPLAY --- INDEED, MANY OF THE BRIGHTEST SUPERNOVAE EVER RECORDED ARE THOUGHT TO ARISE FROM CIRCUMSTELLAR INTERACTION. IN ORDER TO UNDERSTAND THE PROPERTIES OF THE PROGENITOR STAR AND THE DETAILS OF THE CIRCUMSTELLAR INTERACTION, THERE IS A NEED FOR THEORETICAL MODELS OF INTERACTING SUPERNOVAE. THESE SIMULATED COMPUTER SPECTRA CAN BE DIRECTLY COMPARED TO THE SPECTRA OBSERVED BY TELESCOPES. THESE MODELS ALLOW US TO PROBE THE PHYSICAL CIRCUMSTANCES WHICH UNDERLIE THE OBSERVATIONS. THE SPECTRA OF INTERACTING SUPERNOVAE ARE DOMINATED BY STRONG, NARROW EMISSION LINES OF LIGHT ELEMENTS SUCH AS HYDROGEN AND HELIUM. THESE NARROW LINES GIVE TYPE IIN SUPERNOVAE THEIR DESIGNATION. SIMILARLY, OBJECTS OF TYPE IAN, IBN, ICN, AND IIN ARE SOMEWHAT DISTINCT, BUT ARE ALL DEFINED BY THE NARROW EMISSION LINES THAT RESULT FROM THE INTERACTION OF THEIR EXPANDING ENVELOPES WITH THEIR SURROUNDINGS. THE PHOTOSPHERE IN THESE SUPERNOVAE IS FORMED IN THE MATERIAL ACCRETED DURING THE COASTING PHASE, AND MOST OF THE LUMINOSITY HAS ITS ORIGIN FROM THE CONVERSION OF KINETIC EXPLOSION ENERGY INTO LUMINOSITY. BOTH THERMONUCLEAR TYPE IA AND CORE-COLLAPSE TYPES IB/IC AND II SUPERNOVAE MAY BE THE INNER ENGINE. IN FACT, SEVERAL TYPE IIN SUPERNOVAE AT EARLY TIMES HAVE LATER BEEN CLASSIFIED AS TYPE IA, TYPE IB/C, OR TYPE II AS THEIR SPECTRA REVEAL MORE DETAILS ABOUT THE NATURE OF THE CENTRAL EXPLOSION. AS A RESULT OF THE DOMINANCE OF THE INTERACTION, MODELS OF INTERACTING SUPERNOVAE MUST TAKE INTO ACCOUNT DESCRIPTIONS OF THE HYDRODYNAMICAL, IONIZATION, AND LIGHT FRONTS: A FULL RADIATIONHYDRODYNAMICAL PROBLEM. THE LOW DENSITIES IMPLY STRONG DEPARTURES FROM THERMODYNAMIC EQUILIBRIUM AND, THUS, DEMAND A NON-LTE TREATMENT IN THE RADIATIVE TRANSFER CALCULATION. WE PROPOSE A COLLABORATION BETWEEN THE UNIVERSITY OF OKLAHOMA (OU) AND FLORIDA STATE UNIVERSITY (FSU) TO CALCULATE HYDRODYNAMICAL MODELS, LIGHT CURVES, AND NLTE SPECTRA OF CIRCUMSTELLAR INTERACTING SUPERNOVAE. WE WILL PARAMETERIZE THE EXPLOSION OF A MASSIVE STAR, STUDY THE HYDRODYNAMICAL IMPACT ONTO A CIRCUMSTELLAR MEDIUM AND CALCULATE LIGHT CURVES AND SPECTRA. DIRECT COMPARISON WITH OBSERVED SUPERNOVAE WITH GIVE US DETAILED INFORMATION ON THE PROGENITOR STAR, ITS MASS LOSS HISTORY, AND THE NATURE OF BINARY STELLAR EVOLUTION. WE WILL CALCULATE EXPLOSION MODELS FOR SOME OF THE STELLAR STRUCTURES AND THE ONGOING INTERACTION WITH THE CIRCUMSTELLAR MATERIAL USING OUR RADIATION HYDRO CODE HYDRA AND NLTE GENERALIZED MODEL ATMOSPHERES CODE PHOENIX. WE INTEND TO FOCUS ON THE PHYSICS OF INTERACTING SUPERNOVAE, GOING BEYOND THE REGIME WHERE SELFSIMILAR SOLUTIONS AND PHENOMENOLOGICAL APPROACHES ARE VALID. THIS WILL LIMIT THE PARAMETER SPACE THAT NEEDS TO BE EXAMINED, WHILE STILL ALLOWING FOR DIRECT COMPARISON WITH OBSERVATIONS. SINCE MANY INTERACTING SUPERNOVAE ARE EXTREMELY BRIGHT, THEY CAN BE SEEN AT THE HIGHEST REDSHIFTS AND ARE GOOD PROBES OF THE DARKAGES. THESE SUPERNOVAE WILL BE WELL OBSERVED BY UPCOMING NASA MISSION JWST AS WELL AS GROUND BASED SURVEYS SUCH AS LSST. THE TOOLS FOR THIS WORK ARE IN PLACE: FSU PI PETER HOEFLICH HAS BEEN DEVELOPING AND USING THE HYDRODYNAMIC CODE HYDRA FOR OVER TWO DECADES AND PI EDDIE BARON (OU) HAS BEEN DEVELOPING THE GENERALIZED STELLAR ATMOSPHERE CODE PHOENIX OVER THE SAME TIME PERIOD. BARON AND HOEFLICH HAVE A GOOD WORKING RELATIONSHIP AND HAVE CROSS COMPARED OUR CODES. Funding Only Action ($161) 10/19/20 3 INTERACTING SUPERNOVAE ARE POORLY-UNDERSTOOD ASTRONOMICAL EVENTS WITH GREAT POTENTIAL FOR EXPANDING OUR UNDERSTANDING OF HOW STARS EVOLVE AND DIE, AND COULD PROVIDE IMPORTANT CLUES ABOUT THE EARLY FORMATION OF LARGE- SCALE STRUCTURES SUCH AS GALAXIES IN THE UNIVERSE. INTERACTING SUPERNOVAE OCCUR WHEN A STAR EXPLODES WITHIN A DENSE CLOUD OF MATERIAL SHED FROM THE STAR IN THE COURSE OF ITS EVOLUTION. THE RESULTING VIOLENT INTERACTION BETWEEN THE EXPANDING SUPERNOVA EXPLOSION AND THE CLOUD OF CIRCUMSTELLAR MATERIAL CAN LEAD TO AN ENORMOUSLY BRIGHT VISUAL DISPLAY --- INDEED, MANY OF THE BRIGHTEST SUPERNOVAE EVER RECORDED ARE THOUGHT TO ARISE FROM CIRCUMSTELLAR INTERACTION. IN ORDER TO UNDERSTAND THE PROPERTIES OF THE PROGENITOR STAR AND THE DETAILS OF THE CIRCUMSTELLAR INTERACTION, THERE IS A NEED FOR THEORETICAL MODELS OF INTERACTING SUPERNOVAE. THESE SIMULATED COMPUTER SPECTRA CAN BE DIRECTLY COMPARED TO THE SPECTRA OBSERVED BY TELESCOPES. THESE MODELS ALLOW US TO PROBE THE PHYSICAL CIRCUMSTANCES WHICH UNDERLIE THE OBSERVATIONS. THE SPECTRA OF INTERACTING SUPERNOVAE ARE DOMINATED BY STRONG, NARROW EMISSION LINES OF LIGHT ELEMENTS SUCH AS HYDROGEN AND HELIUM. THESE NARROW LINES GIVE TYPE IIN SUPERNOVAE THEIR DESIGNATION. SIMILARLY, OBJECTS OF TYPE IAN, IBN, ICN, AND IIN ARE SOMEWHAT DISTINCT, BUT ARE ALL DEFINED BY THE NARROW EMISSION LINES THAT RESULT FROM THE INTERACTION OF THEIR EXPANDING ENVELOPES WITH THEIR SURROUNDINGS. THE PHOTOSPHERE IN THESE SUPERNOVAE IS FORMED IN THE MATERIAL ACCRETED DURING THE COASTING PHASE, AND MOST OF THE LUMINOSITY HAS ITS ORIGIN FROM THE CONVERSION OF KINETIC EXPLOSION ENERGY INTO LUMINOSITY. BOTH THERMONUCLEAR TYPE IA AND CORE-COLLAPSE TYPES IB/IC AND II SUPERNOVAE MAY BE THE INNER ENGINE. IN FACT, SEVERAL TYPE IIN SUPERNOVAE AT EARLY TIMES HAVE LATER BEEN CLASSIFIED AS TYPE IA, TYPE IB/C, OR TYPE II AS THEIR SPECTRA REVEAL MORE DETAILS ABOUT THE NATURE OF THE CENTRAL EXPLOSION. AS A RESULT OF THE DOMINANCE OF THE INTERACTION, MODELS OF INTERACTING SUPERNOVAE MUST TAKE INTO ACCOUNT DESCRIPTIONS OF THE HYDRODYNAMICAL, IONIZATION, AND LIGHT FRONTS: A FULL RADIATIONHYDRODYNAMICAL PROBLEM. THE LOW DENSITIES IMPLY STRONG DEPARTURES FROM THERMODYNAMIC EQUILIBRIUM AND, THUS, DEMAND A NON-LTE TREATMENT IN THE RADIATIVE TRANSFER CALCULATION. WE PROPOSE A COLLABORATION BETWEEN THE UNIVERSITY OF OKLAHOMA (OU) AND FLORIDA STATE UNIVERSITY (FSU) TO CALCULATE HYDRODYNAMICAL MODELS, LIGHT CURVES, AND NLTE SPECTRA OF CIRCUMSTELLAR INTERACTING SUPERNOVAE. WE WILL PARAMETERIZE THE EXPLOSION OF A MASSIVE STAR, STUDY THE HYDRODYNAMICAL IMPACT ONTO A CIRCUMSTELLAR MEDIUM AND CALCULATE LIGHT CURVES AND SPECTRA. DIRECT COMPARISON WITH OBSERVED SUPERNOVAE WITH GIVE US DETAILED INFORMATION ON THE PROGENITOR STAR, ITS MASS LOSS HISTORY, AND THE NATURE OF BINARY STELLAR EVOLUTION. WE WILL CALCULATE EXPLOSION MODELS FOR SOME OF THE STELLAR STRUCTURES AND THE ONGOING INTERACTION WITH THE CIRCUMSTELLAR MATERIAL USING OUR RADIATION HYDRO CODE HYDRA AND NLTE GENERALIZED MODEL ATMOSPHERES CODE PHOENIX. WE INTEND TO FOCUS ON THE PHYSICS OF INTERACTING SUPERNOVAE, GOING BEYOND THE REGIME WHERE SELFSIMILAR SOLUTIONS AND PHENOMENOLOGICAL APPROACHES ARE VALID. THIS WILL LIMIT THE PARAMETER SPACE THAT NEEDS TO BE EXAMINED, WHILE STILL ALLOWING FOR DIRECT COMPARISON WITH OBSERVATIONS. SINCE MANY INTERACTING SUPERNOVAE ARE EXTREMELY BRIGHT, THEY CAN BE SEEN AT THE HIGHEST REDSHIFTS AND ARE GOOD PROBES OF THE DARKAGES. THESE SUPERNOVAE WILL BE WELL OBSERVED BY UPCOMING NASA MISSION JWST AS WELL AS GROUND BASED SURVEYS SUCH AS LSST. THE TOOLS FOR THIS WORK ARE IN PLACE: FSU PI PETER HOEFLICH HAS BEEN DEVELOPING AND USING THE HYDRODYNAMIC CODE HYDRA FOR OVER TWO DECADES AND PI EDDIE BARON (OU) HAS BEEN DEVELOPING THE GENERALIZED STELLAR ATMOSPHERE CODE PHOENIX OVER THE SAME TIME PERIOD. BARON AND HOEFLICH HAVE A GOOD WORKING RELATIONSHIP AND HAVE CROSS COMPARED OUR CODES. Other Administrative Action $0 10/3/18 Not listed INTERACTING SUPERNOVAE ARE POORLY-UNDERSTOOD ASTRONOMICAL EVENTS WITH GREAT POTENTIAL FOR EXPANDING OUR UNDERSTANDING OF HOW STARS EVOLVE AND DIE AND COULD PROVIDE IMPORTANT CLUES ABOUT THE EARLY FORMATION OF LARGE-SCALE STRUCTURES SUCH AS GALAXIES IN THE UNIVERSE. INTERACTING SUPERNOVAE OCCUR WHEN A STAR EXPLODES WITHIN A DENSE CLOUD OF MATERIAL SHED FROM THE STAR IN THE COURSE OF ITS EVOLUTION. THE RESULTING VIOLENT INTERACTION BETWEEN THE EXPANDING SUPERNOVA EXPLOSION AND THE CLOUD OF CIRCUMSTELLAR MATERIAL CAN LEAD TO AN ENORMOUSLY BRIGHT VISUAL DISPLAY --- INDEED MANY OF THE BRIGHTEST SUPERNOVAE EVER RECORDED ARE THOUGHT TO ARISE FROM CIRCUMSTELLAR INTERACTION. IN ORDER TO UNDERSTAND THE PROPERTIES OF THE PROGENITOR STAR AND THE DETAILS OF THE CIRCUMSTELLAR INTERACTION THERE IS A NEED FOR THEORETICAL MODELS OF INTERACTING SUPERNOVAE. THESE SIMULATED COMPUTER SPECTRA CAN BE DIRECTLY COMPARED TO THE SPECTRA OBSERVED BY TELESCOPES. THESE MODELS ALLOW US TO PROBE THE PHYSICAL CIRCUMSTANCES WHICH UNDERLIE THE OBSERVATIONS. THE SPECTRA OF INTERACTING SUPERNOVAE ARE DOMINATED BY STRONG NARROW EMISSION LINES OF LIGHT ELEMENTS SUCH AS HYDROGEN AND HELIUM. THESE NARROW LINES GIVE TYPE IIN SUPERNOVAE THEIR DESIGNATION. SIMILARLY OBJECTS OF TYPE IAN IBN ICN AND IIN ARE SOMEWHAT DISTINCT BUT ARE ALL DEFINED BY THE NARROW EMISSION LINES THAT RESULT FROM THE INTERACTION OF THEIR EXPANDING ENVELOPES WITH THEIR SURROUNDINGS. THE PHOTOSPHERE IN THESE SUPERNOVAE IS FORMED IN THE MATERIAL ACCRETED DURING THE COASTING PHASE AND MOST OF THE LUMINOSITY HAS ITS ORIGIN FROM THE CONVERSION OF KINETIC EXPLOSION ENERGY INTO LUMINOSITY. BOTH THERMONUCLEAR TYPE IA AND CORE-COLLAPSE TYPES IB/IC AND II SUPERNOVAE MAY BE THE INNER ENGINE. IN FACT SEVERAL TYPE IIN SUPERNOVAE AT EARLY TIMES HAVE LATER BEEN CLASSIFIED AS TYPE IA TYPE IB/C OR TYPE II AS THEIR SPECTRA REVEAL MORE DETAILS ABOUT THE NATURE OF THE CENTRAL EXPLOSION. AS A RESULT OF THE DOMINANCE OF THE INTERACTION MODELS OF INTERACTING SUPERNOVAE MUST TAKE INTO ACCOUNT DESCRIPTIONS OF THE HYDRODYNAMICAL IONIZATION AND LIGHT FRONTS: A FULL RADIATIONHYDRODYNAMICAL PROBLEM. THE LOW DENSITIES IMPLY STRONG DEPARTURES FROM THERMODYNAMIC EQUILIBRIUM AND THUS DEMAND A NON-LTE TREATMENT IN THE RADIATIVE TRANSFER CALCULATION. WE PROPOSE A COLLABORATION BETWEEN THE UNIVERSITY OF OKLAHOMA (OU) AND FLORIDA STATE UNIVERSITY (FSU) TO CALCULATE HYDRODYNAMICAL MODELS LIGHT CURVES AND NLTE SPECTRA OF CIRCUMSTELLAR INTERACTING SUPERNOVAE. WE WILL PARAMETERIZE THE EXPLOSION OF A MASSIVE STAR STUDY THE HYDRODYNAMICAL IMPACT ONTO A CIRCUMSTELLAR MEDIUM AND CALCULATE LIGHT CURVES AND SPECTRA. DIRECT COMPARISON WITH OBSERVED SUPERNOVAE WITH GIVE US DETAILED INFORMATION ON THE PROGENITOR STAR ITS MASS LOSS HISTORY AND THE NATURE OF BINARY STELLAR EVOLUTION. WE WILL CALCULATE EXPLOSION MODELS FOR SOME OF THE STELLARSTRUCTURES AND THE ONGOING INTERACTION WITH THE CIRCUMSTELLAR MATERIAL USING OUR RADIATION HYDRO CODE HYDRA AND NLTE GENERALIZED MODEL ATMOSPHERES CODE PHOENIX. WE INTEND TO FOCUS ON THE PHYSICS OF INTERACTING SUPERNOVAE GOING BEYOND THE REGIME WHERE SELFSIMILAR SOLUTIONS AND PHENOMENOLOGICAL APPROACHES ARE VALID. THIS WILL LIMIT THE PARAMETER SPACE THAT NEEDS TO BE EXAMINED WHILE STILL ALLOWING FOR DIRECT COMPARISON WITH OBSERVATIONS. SINCE MANY INTERACTING SUPERNOVAE ARE EXTREMELY BRIGHT THEY CAN BE SEEN AT THE HIGHEST REDSHIFTS AND ARE GOOD PROBES OF THE DARKAGES. THESE SUPERNOVAE WILL BE WELL OBSERVED BY UPCOMING NASA MISSION JWST AS WELL AS GROUND BASED SURVEYS SUCH AS LSST. THE TOOLS FOR THIS WORK ARE IN PLACE: FSU PI PETER HOEFLICH HAS BEEN DEVELOPING AND USING THE HYDRODYNAMIC CODE HYDRA FOR OVER TWO DECADES AND PI EDDIE BARON (OU) HAS BEEN DEVELOPING THE GENERALIZED STELLAR ATMOSPHERE CODE PHOENIX OVER THE SAME TIME PERIOD. BARON AND HOEFLICH HAVE A GOOD WORKING RELATIONSHIP AND HAVE CROSS COMPARED OUR CODES. $0 10/3/18 2 INTERACTING SUPERNOVAE ARE POORLY-UNDERSTOOD ASTRONOMICAL EVENTS WITH GREAT POTENTIAL FOR EXPANDING OUR UNDERSTANDING OF HOW STARS EVOLVE AND DIE, AND COULD PROVIDE IMPORTANT CLUES ABOUT THE EARLY FORMATION OF LARGE- SCALE STRUCTURES SUCH AS GALAXIES IN THE UNIVERSE. INTERACTING SUPERNOVAE OCCUR WHEN A STAR EXPLODES WITHIN A DENSE CLOUD OF MATERIAL SHED FROM THE STAR IN THE COURSE OF ITS EVOLUTION. THE RESULTING VIOLENT INTERACTION BETWEEN THE EXPANDING SUPERNOVA EXPLOSION AND THE CLOUD OF CIRCUMSTELLAR MATERIAL CAN LEAD TO AN ENORMOUSLY BRIGHT VISUAL DISPLAY --- INDEED, MANY OF THE BRIGHTEST SUPERNOVAE EVER RECORDED ARE THOUGHT TO ARISE FROM CIRCUMSTELLAR INTERACTION. IN ORDER TO UNDERSTAND THE PROPERTIES OF THE PROGENITOR STAR AND THE DETAILS OF THE CIRCUMSTELLAR INTERACTION, THERE IS A NEED FOR THEORETICAL MODELS OF INTERACTING SUPERNOVAE. THESE SIMULATED COMPUTER SPECTRA CAN BE DIRECTLY COMPARED TO THE SPECTRA OBSERVED BY TELESCOPES. THESE MODELS ALLOW US TO PROBE THE PHYSICAL CIRCUMSTANCES WHICH UNDERLIE THE OBSERVATIONS. THE SPECTRA OF INTERACTING SUPERNOVAE ARE DOMINATED BY STRONG, NARROW EMISSION LINES OF LIGHT ELEMENTS SUCH AS HYDROGEN AND HELIUM. THESE NARROW LINES GIVE TYPE IIN SUPERNOVAE THEIR DESIGNATION. SIMILARLY, OBJECTS OF TYPE IAN, IBN, ICN, AND IIN ARE SOMEWHAT DISTINCT, BUT ARE ALL DEFINED BY THE NARROW EMISSION LINES THAT RESULT FROM THE INTERACTION OF THEIR EXPANDING ENVELOPES WITH THEIR SURROUNDINGS. THE PHOTOSPHERE IN THESE SUPERNOVAE IS FORMED IN THE MATERIAL ACCRETED DURING THE COASTING PHASE, AND MOST OF THE LUMINOSITY HAS ITS ORIGIN FROM THE CONVERSION OF KINETIC EXPLOSION ENERGY INTO LUMINOSITY. BOTH THERMONUCLEAR TYPE IA AND CORE-COLLAPSE TYPES IB/IC AND II SUPERNOVAE MAY BE THE INNER ENGINE. IN FACT, SEVERAL TYPE IIN SUPERNOVAE AT EARLY TIMES HAVE LATER BEEN CLASSIFIED AS TYPE IA, TYPE IB/C, OR TYPE II AS THEIR SPECTRA REVEAL MORE DETAILS ABOUT THE NATURE OF THE CENTRAL EXPLOSION. AS A RESULT OF THE DOMINANCE OF THE INTERACTION, MODELS OF INTERACTING SUPERNOVAE MUST TAKE INTO ACCOUNT DESCRIPTIONS OF THE HYDRODYNAMICAL, IONIZATION, AND LIGHT FRONTS: A FULL RADIATIONHYDRODYNAMICAL PROBLEM. THE LOW DENSITIES IMPLY STRONG DEPARTURES FROM THERMODYNAMIC EQUILIBRIUM AND, THUS, DEMAND A NON-LTE TREATMENT IN THE RADIATIVE TRANSFER CALCULATION. WE PROPOSE A COLLABORATION BETWEEN THE UNIVERSITY OF OKLAHOMA (OU) AND FLORIDA STATE UNIVERSITY (FSU) TO CALCULATE HYDRODYNAMICAL MODELS, LIGHT CURVES, AND NLTE SPECTRA OF CIRCUMSTELLAR INTERACTING SUPERNOVAE. WE WILL PARAMETERIZE THE EXPLOSION OF A MASSIVE STAR, STUDY THE HYDRODYNAMICAL IMPACT ONTO A CIRCUMSTELLAR MEDIUM AND CALCULATE LIGHT CURVES AND SPECTRA. DIRECT COMPARISON WITH OBSERVED SUPERNOVAE WITH GIVE US DETAILED INFORMATION ON THE PROGENITOR STAR, ITS MASS LOSS HISTORY, AND THE NATURE OF BINARY STELLAR EVOLUTION. WE WILL CALCULATE EXPLOSION MODELS FOR SOME OF THE STELLAR STRUCTURES AND THE ONGOING INTERACTION WITH THE CIRCUMSTELLAR MATERIAL USING OUR RADIATION HYDRO CODE HYDRA AND NLTE GENERALIZED MODEL ATMOSPHERES CODE PHOENIX. WE INTEND TO FOCUS ON THE PHYSICS OF INTERACTING SUPERNOVAE, GOING BEYOND THE REGIME WHERE SELFSIMILAR SOLUTIONS AND PHENOMENOLOGICAL APPROACHES ARE VALID. THIS WILL LIMIT THE PARAMETER SPACE THAT NEEDS TO BE EXAMINED, WHILE STILL ALLOWING FOR DIRECT COMPARISON WITH OBSERVATIONS. SINCE MANY INTERACTING SUPERNOVAE ARE EXTREMELY BRIGHT, THEY CAN BE SEEN AT THE HIGHEST REDSHIFTS AND ARE GOOD PROBES OF THE DARKAGES. THESE SUPERNOVAE WILL BE WELL OBSERVED BY UPCOMING NASA MISSION JWST AS WELL AS GROUND BASED SURVEYS SUCH AS LSST. THE TOOLS FOR THIS WORK ARE IN PLACE: FSU PI PETER HOEFLICH HAS BEEN DEVELOPING AND USING THE HYDRODYNAMIC CODE HYDRA FOR OVER TWO DECADES AND PI EDDIE BARON (OU) HAS BEEN DEVELOPING THE GENERALIZED STELLAR ATMOSPHERE CODE PHOENIX OVER THE SAME TIME PERIOD. BARON AND HOEFLICH HAVE A GOOD WORKING RELATIONSHIP AND HAVE CROSS COMPARED OUR CODES. Funding Only Action $124.7k 11/24/17