Not listed WE PROPOSE TO BUILD A VERSATILE SET OF SELF-CONSISTENT ATMOSPHERIC MODELS FOR HOT ROCKY EXOPLANETS AND USE THEM TO PREDICT THEIR TRANSIT AND ECLIPSE SPECTRA. HOT ROCKY EXOPLANETS WILL FORM THE MAJORITY OF SMALL PLANETS IN CLOSE-IN ORBITS TO BE DISCOVERED BY THE TESS AND KEPLER K2 MISSIONS AND OFFER THE BEST OPPORTUNITY FOR CHARACTERIZATION WITH CURRENT AND FUTURE INSTRUMENTS. WE WILL USE FULLY NONGREY RADIATIVE-CONVECTIVE ATMOSPHERIC STRUCTURE CODES WITH CLOUD FORMATION AND VERTICAL MIXING COMBINED WITH A SELF-CONSISTENT TREATMENT OF GAS CHEMISTRY ABOVE THE MAGMA OCEAN. BEING IN EQUILIBRIUM WITH THE SURFACE THE VAPORIZED ROCK MATERIAL CAN BE A GOOD TRACER OF THE BULK COMPOSITION OF THE PLANET. WE WILL DERIVE THE ATMOSPHERIC STRUCTURE AND ESCAPE RATES CONSIDERING BOTH VOLATILEFREE AND VOLATILE BEARING COMPOSITIONS WHICH REFLECT THE DIVERSITY OF HOT ROCKY PLANET ATMOSPHERES. OUR MODELS WILL INFORM FOLLOWUP OBSERVATIONS WITH JWST AND GROUND-BASED INSTRUMENTS AID THE INTERPRETATION OF TRANSIT AND ECLIPSE SPECTRA AND PROVIDE A BETTER UNDERSTANDING OF VOLATILE LOSS IN THESE ATMOSPHERES. SUCH RESULTS WILL HELP REFINE OUR PICTURE OF ROCKY PLANET FORMATION AND EVOLUTION. PLANETS IN ULTRA-SHORT PERIOD (USP) ORBITS ARE A SPECIAL CLASS OF HOT ROCKY EXOPLANETS. AS SHOWN BY KEPLER THESE PLANETS ARE GENERALLY SMALLER THAN 2 EARTH RADII SUGGESTING THAT THEY ARE LIKELY TO BE ROCKY AND COULD HAVE LOST THEIR VOLATILES THROUGH PHOTO-EVAPORATION. BEING CLOSE TO THEIR HOST STARS THESE PLANETS ARE ULTRA-HOT WITH ESTIMATED TEMPERATURES OF 1000-3000 K. A NUMBER OF USP PLANETS HAVE BEEN ALREADY DISCOVERED (E.G. KEPLER-78 B COROT-7 B KEPLER-10 B) AND THIS NUMBER IS EXPECTED TO GROW BY ING ADDITIONAL PLANET CANDIDATES. THE CHARACTERIZATION OF PLANETS ON ULTRA-SHORT ORBITS IS ADVANTAGEOUS DUE TO THE LARGER NUMBER OF OBSERVABLE TRANSITS AND THE LARGER TRANSIT SIGNAL IN THE CASE OF AN EVAPORATING ATMOSPHERE. MUCH ADVANCE HAS BEEN MADE IN UNDERSTANDING AND CHARACTERIZING HOT JUPITERS IN SIMILAR TRANSIT CONFIGURATIONS. FOR EXAMPLE NA HAS BEEN THE FIRST SPECIES TO BE DETECTED IN AN EXOPLANET ATMOSPHERE BY OBSERVING THE EVAPORATING HOT-JUPITER HD209458B. UNDERSTANDING THE INTERPLAY BETWEEN THE MAGMA OUTGASSING AND VOLATILE LOSS WILL BE AN IMPORTANT PART OF THIS PROJECT. OUR TEAM HAS THE EXPERTISE IN THE CHEMISTRY RADIATIVE TRANSFER AND ATMOSPHERIC ESCAPE MODELING AT THESE EXOTIC TEMPERATURES. OUR RECENT WORK HAS ANALYZED THE EMERGING ATMOSPHERES OF TERRESTRIAL PLANETS AFTER GIANT IMPACTS USING A WELL-ESTABLISHED RADIATIVECONVECTIVE ATMOSPHERIC STRUCTURE CODE WITH AN EXTENSIVE OPACITY DATABASE FOR ALL RELEVANT MOLECULES AND THE CHEMISTRY SELF-CONSISTENTLY CALCULATED FOR CONTINENTAL CRUST AND BULK SILICATE EARTH COMPOSITIONS. WE WILL EXPAND ON THIS WORK BY CONSIDERING A WIDER RANGE OF CHEMICAL COMPOSITIONS ASSESSING THE IMPORTANCE OF CLOUDS AND GENERATING CLOUDY MODELS AND DEVELOPING DIS-EQUILIBRIUM MODELS BY TAKING INTO ACCOUNT VERTICAL MIXING AND PHOTOCHEMISTRY. PHOTO-EVAPORATION WILL BE CONSIDERED IN THE ENERGY BALANCE BETWEEN HEATING COOLING AND MASS LOSS. WE ALSO HAVE IN-HOUSE CODES TO GENERATE HIGH-RESOLUTION ECLIPSE SPECTRA AND PREDICT TRANSIT DEPTHS AND OBSERVABLE SIGNATURES. THE DEVELOPMENT OF THE ATMOSPHERIC CODE THE MOLECULAR OPACITY UPDATES THE ATMOSPHERIC STRUCTURE CALCULATIONS AND THE HIGH RESOLUTION ECLIPSE SPECTRA WILL BE PERFORMED BY R. LUPU M. MARLEY AND R. FREEDMAN AT NASA AMES. THE ATMOSPHERIC CHEMISTRY GRIDS WILL BE PROVIDED BY B. FEGLEY AND K. LODDERS AT WASHINGTON UNIVERSITY. THE TRANSIT SPECTRA AND OBSERVATIONAL FEATURES WILL BE COMPUTED BY J. FORTNEY AT UCSC AND THE ATMOSPHERIC ESCAPE CALCULATIONS WILL BE PERFORMED BY K. ZAHNLE AT NASA AMES. THIS PROPOSAL ADDRESSES THE FOLLOWING GOALS OF THE EXOPLANET RESEARCH PROGRAM: EXPLAIN OBSERVATIONS OF EXOPLANETARY SYSTEMS AND UNDERSTAND THE CHEMICAL AND PHYSICAL PROCESSES OF EXOPLANETS. OUR RESULTS WILL ALSO INFORM FUTURE JWST OBSERVATIONS. ($31k) 6/15/22 10 WE PROPOSE TO BUILD A VERSATILE SET OF SELF-CONSISTENT ATMOSPHERIC MODELS FOR HOT ROCKY EXOPLANETS AND USE THEM TO PREDICT THEIR TRANSIT AND ECLIPSE SPECTRA. HOT ROCKY EXOPLANETS WILL FORM THE MAJORITY OF SMALL PLANETS IN CLOSE-IN ORBITS TO BE DISCOVERED BY THE TESS AND KEPLER K2 MISSIONS, AND OFFER THE BEST OPPORTUNITY FOR CHARACTERIZATION WITH CURRENT AND FUTURE INSTRUMENTS. WE WILL USE FULLY NONGREY RADIATIVE-CONVECTIVE ATMOSPHERIC STRUCTURE CODES WITH CLOUD FORMATION AND VERTICAL MIXING, COMBINED WITH A SELF-CONSISTENT TREATMENT OF GAS CHEMISTRY ABOVE THE MAGMA OCEAN. BEING IN EQUILIBRIUM WITH THE SURFACE, THE VAPORIZED ROCK MATERIAL CAN BE A GOOD TRACER OF THE BULK COMPOSITION OF THE PLANET. WE WILL DERIVE THE ATMOSPHERIC STRUCTURE AND ESCAPE RATES CONSIDERING BOTH VOLATILEFREE AND VOLATILE BEARING COMPOSITIONS, WHICH REFLECT THE DIVERSITY OF HOT ROCKY PLANET ATMOSPHERES. OUR MODELS WILL INFORM FOLLOWUP OBSERVATIONS WITH JWST AND GROUND-BASED INSTRUMENTS, AID THE INTERPRETATION OF TRANSIT AND ECLIPSE SPECTRA, AND PROVIDE A BETTER UNDERSTANDING OF VOLATILE LOSS IN THESE ATMOSPHERES. SUCH RESULTS WILL HELP REFINE OUR PICTURE OF ROCKY PLANET FORMATION AND EVOLUTION. PLANETS IN ULTRA-SHORT PERIOD (USP) ORBITS ARE A SPECIAL CLASS OF HOT ROCKY EXOPLANETS. AS SHOWN BY KEPLER, THESE PLANETS ARE GENERALLY SMALLER THAN 2 EARTH RADII, SUGGESTING THAT THEY ARE LIKELY TO BE ROCKY AND COULD HAVE LOST THEIR VOLATILES THROUGH PHOTO-EVAPORATION. BEING CLOSE TO THEIR HOST STARS, THESE PLANETS ARE ULTRA-HOT, WITH ESTIMATED TEMPERATURES OF 1000-3000 K. A NUMBER OF USP PLANETS HAVE BEEN ALREADY DISCOVERED (E.G. KEPLER-78 B, COROT-7 B, KEPLER-10 B), AND THIS NUMBER IS EXPECTED TO GROW BY ING ADDITIONAL PLANET CANDIDATES. THE CHARACTERIZATION OF PLANETS ON ULTRA-SHORT ORBITS IS ADVANTAGEOUS DUE TO THE LARGER NUMBER OF OBSERVABLE TRANSITS, AND THE LARGER TRANSIT SIGNAL IN THE CASE OF AN EVAPORATING ATMOSPHERE. MUCH ADVANCE HAS BEEN MADE IN UNDERSTANDING AND CHARACTERIZING HOT JUPITERS IN SIMILAR TRANSIT CONFIGURATIONS. FOR EXAMPLE, NA HAS BEEN THE FIRST SPECIES TO BE DETECTED IN AN EXOPLANET ATMOSPHERE, BY OBSERVING THE EVAPORATING HOT-JUPITER HD209458B. UNDERSTANDING THE INTERPLAY BETWEEN THE MAGMA OUTGASSING AND VOLATILE LOSS WILL BE AN IMPORTANT PART OF THIS PROJECT. OUR TEAM HAS THE EXPERTISE IN THE CHEMISTRY, RADIATIVE TRANSFER, AND ATMOSPHERIC ESCAPE MODELING AT THESE EXOTIC TEMPERATURES. OUR RECENT WORK HAS ANALYZED THE EMERGING ATMOSPHERES OF TERRESTRIAL PLANETS AFTER GIANT IMPACTS, USING A WELL-ESTABLISHED RADIATIVECONVECTIVE ATMOSPHERIC STRUCTURE CODE, WITH AN EXTENSIVE OPACITY DATABASE FOR ALL RELEVANT MOLECULES, AND THE CHEMISTRY SELF-CONSISTENTLY CALCULATED FOR CONTINENTAL CRUST AND BULK SILICATE EARTH COMPOSITIONS. WE WILL EXPAND ON THIS WORK BY CONSIDERING A WIDER RANGE OF CHEMICAL COMPOSITIONS, ASSESSING THE IMPORTANCE OF CLOUDS AND GENERATING CLOUDY MODELS, AND DEVELOPING DIS-EQUILIBRIUM MODELS BY TAKING INTO ACCOUNT VERTICAL MIXING AND PHOTOCHEMISTRY. PHOTO-EVAPORATION WILL BE CONSIDERED IN THE ENERGY BALANCE BETWEEN HEATING, COOLING AND MASS LOSS. WE ALSO HAVE IN-HOUSE CODES TO GENERATE HIGH-RESOLUTION ECLIPSE SPECTRA AND PREDICT TRANSIT DEPTHS AND OBSERVABLE SIGNATURES. THE DEVELOPMENT OF THE ATMOSPHERIC CODE, THE MOLECULAR OPACITY UPDATES, THE ATMOSPHERIC STRUCTURE CALCULATIONS AND THE HIGH RESOLUTION ECLIPSE SPECTRA WILL BE PERFORMED BY R. LUPU, M. MARLEY, AND R. FREEDMAN AT NASA AMES. THE ATMOSPHERIC CHEMISTRY GRIDS WILL BE PROVIDED BY B. FEGLEY AND K. LODDERS AT WASHINGTON UNIVERSITY. THE TRANSIT SPECTRA AND OBSERVATIONAL FEATURES WILL BE COMPUTED BY J. FORTNEY AT UCSC, AND THE ATMOSPHERIC ESCAPE CALCULATIONS WILL BE PERFORMED BY K. ZAHNLE AT NASA AMES. THIS PROPOSAL ADDRESSES THE FOLLOWING GOALS OF THE EXOPLANET RESEARCH PROGRAM: EXPLAIN OBSERVATIONS OF EXOPLANETARY SYSTEMS, AND UNDERSTAND THE CHEMICAL AND PHYSICAL PROCESSES OF EXOPLANETS. OUR RESULTS WILL ALSO INFORM FUTURE JWST OBSERVATIONS. Funding Only Action ($31k) 6/15/22 9 WE PROPOSE TO BUILD A VERSATILE SET OF SELF-CONSISTENT ATMOSPHERIC MODELS FOR HOT ROCKY EXOPLANETS AND USE THEM TO PREDICT THEIR TRANSIT AND ECLIPSE SPECTRA. HOT ROCKY EXOPLANETS WILL FORM THE MAJORITY OF SMALL PLANETS IN CLOSE-IN ORBITS TO BE DISCOVERED BY THE TESS AND KEPLER K2 MISSIONS, AND OFFER THE BEST OPPORTUNITY FOR CHARACTERIZATION WITH CURRENT AND FUTURE INSTRUMENTS. WE WILL USE FULLY NONGREY RADIATIVE-CONVECTIVE ATMOSPHERIC STRUCTURE CODES WITH CLOUD FORMATION AND VERTICAL MIXING, COMBINED WITH A SELF-CONSISTENT TREATMENT OF GAS CHEMISTRY ABOVE THE MAGMA OCEAN. BEING IN EQUILIBRIUM WITH THE SURFACE, THE VAPORIZED ROCK MATERIAL CAN BE A GOOD TRACER OF THE BULK COMPOSITION OF THE PLANET. WE WILL DERIVE THE ATMOSPHERIC STRUCTURE AND ESCAPE RATES CONSIDERING BOTH VOLATILEFREE AND VOLATILE BEARING COMPOSITIONS, WHICH REFLECT THE DIVERSITY OF HOT ROCKY PLANET ATMOSPHERES. OUR MODELS WILL INFORM FOLLOWUP OBSERVATIONS WITH JWST AND GROUND-BASED INSTRUMENTS, AID THE INTERPRETATION OF TRANSIT AND ECLIPSE SPECTRA, AND PROVIDE A BETTER UNDERSTANDING OF VOLATILE LOSS IN THESE ATMOSPHERES. SUCH RESULTS WILL HELP REFINE OUR PICTURE OF ROCKY PLANET FORMATION AND EVOLUTION. PLANETS IN ULTRA-SHORT PERIOD (USP) ORBITS ARE A SPECIAL CLASS OF HOT ROCKY EXOPLANETS. AS SHOWN BY KEPLER, THESE PLANETS ARE GENERALLY SMALLER THAN 2 EARTH RADII, SUGGESTING THAT THEY ARE LIKELY TO BE ROCKY AND COULD HAVE LOST THEIR VOLATILES THROUGH PHOTO-EVAPORATION. BEING CLOSE TO THEIR HOST STARS, THESE PLANETS ARE ULTRA-HOT, WITH ESTIMATED TEMPERATURES OF 1000-3000 K. A NUMBER OF USP PLANETS HAVE BEEN ALREADY DISCOVERED (E.G. KEPLER-78 B, COROT-7 B, KEPLER-10 B), AND THIS NUMBER IS EXPECTED TO GROW BY ING ADDITIONAL PLANET CANDIDATES. THE CHARACTERIZATION OF PLANETS ON ULTRA-SHORT ORBITS IS ADVANTAGEOUS DUE TO THE LARGER NUMBER OF OBSERVABLE TRANSITS, AND THE LARGER TRANSIT SIGNAL IN THE CASE OF AN EVAPORATING ATMOSPHERE. MUCH ADVANCE HAS BEEN MADE IN UNDERSTANDING AND CHARACTERIZING HOT JUPITERS IN SIMILAR TRANSIT CONFIGURATIONS. FOR EXAMPLE, NA HAS BEEN THE FIRST SPECIES TO BE DETECTED IN AN EXOPLANET ATMOSPHERE, BY OBSERVING THE EVAPORATING HOT-JUPITER HD209458B. UNDERSTANDING THE INTERPLAY BETWEEN THE MAGMA OUTGASSING AND VOLATILE LOSS WILL BE AN IMPORTANT PART OF THIS PROJECT. OUR TEAM HAS THE EXPERTISE IN THE CHEMISTRY, RADIATIVE TRANSFER, AND ATMOSPHERIC ESCAPE MODELING AT THESE EXOTIC TEMPERATURES. OUR RECENT WORK HAS ANALYZED THE EMERGING ATMOSPHERES OF TERRESTRIAL PLANETS AFTER GIANT IMPACTS, USING A WELL-ESTABLISHED RADIATIVECONVECTIVE ATMOSPHERIC STRUCTURE CODE, WITH AN EXTENSIVE OPACITY DATABASE FOR ALL RELEVANT MOLECULES, AND THE CHEMISTRY SELF-CONSISTENTLY CALCULATED FOR CONTINENTAL CRUST AND BULK SILICATE EARTH COMPOSITIONS. WE WILL EXPAND ON THIS WORK BY CONSIDERING A WIDER RANGE OF CHEMICAL COMPOSITIONS, ASSESSING THE IMPORTANCE OF CLOUDS AND GENERATING CLOUDY MODELS, AND DEVELOPING DIS-EQUILIBRIUM MODELS BY TAKING INTO ACCOUNT VERTICAL MIXING AND PHOTOCHEMISTRY. PHOTO-EVAPORATION WILL BE CONSIDERED IN THE ENERGY BALANCE BETWEEN HEATING, COOLING AND MASS LOSS. WE ALSO HAVE IN-HOUSE CODES TO GENERATE HIGH-RESOLUTION ECLIPSE SPECTRA AND PREDICT TRANSIT DEPTHS AND OBSERVABLE SIGNATURES. THE DEVELOPMENT OF THE ATMOSPHERIC CODE, THE MOLECULAR OPACITY UPDATES, THE ATMOSPHERIC STRUCTURE CALCULATIONS AND THE HIGH RESOLUTION ECLIPSE SPECTRA WILL BE PERFORMED BY R. LUPU, M. MARLEY, AND R. FREEDMAN AT NASA AMES. THE ATMOSPHERIC CHEMISTRY GRIDS WILL BE PROVIDED BY B. FEGLEY AND K. LODDERS AT WASHINGTON UNIVERSITY. THE TRANSIT SPECTRA AND OBSERVATIONAL FEATURES WILL BE COMPUTED BY J. FORTNEY AT UCSC, AND THE ATMOSPHERIC ESCAPE CALCULATIONS WILL BE PERFORMED BY K. ZAHNLE AT NASA AMES. THIS PROPOSAL ADDRESSES THE FOLLOWING GOALS OF THE EXOPLANET RESEARCH PROGRAM: EXPLAIN OBSERVATIONS OF EXOPLANETARY SYSTEMS, AND UNDERSTAND THE CHEMICAL AND PHYSICAL PROCESSES OF EXOPLANETS. OUR RESULTS WILL ALSO INFORM FUTURE JWST OBSERVATIONS. Other Administrative Action $0 1/13/21 Not listed WE PROPOSE TO BUILD A VERSATILE SET OF SELF-CONSISTENT ATMOSPHERIC MODELS FOR HOT ROCKY EXOPLANETS AND USE THEM TO PREDICT THEIR TRANSIT AND ECLIPSE SPECTRA. HOT ROCKY EXOPLANETS WILL FORM THE MAJORITY OF SMALL PLANETS IN CLOSE-IN ORBITS TO BE DISCOVERED BY THE TESS AND KEPLER K2 MISSIONS AND OFFER THE BEST OPPORTUNITY FOR CHARACTERIZATION WITH CURRENT AND FUTURE INSTRUMENTS. WE WILL USE FULLY NONGREY RADIATIVE-CONVECTIVE ATMOSPHERIC STRUCTURE CODES WITH CLOUD FORMATION AND VERTICAL MIXING COMBINED WITH A SELF-CONSISTENT TREATMENT OF GAS CHEMISTRY ABOVE THE MAGMA OCEAN. BEING IN EQUILIBRIUM WITH THE SURFACE THE VAPORIZED ROCK MATERIAL CAN BE A GOOD TRACER OF THE BULK COMPOSITION OF THE PLANET. WE WILL DERIVE THE ATMOSPHERIC STRUCTURE AND ESCAPE RATES CONSIDERING BOTH VOLATILEFREE AND VOLATILE BEARING COMPOSITIONS WHICH REFLECT THE DIVERSITY OF HOT ROCKY PLANET ATMOSPHERES. OUR MODELS WILL INFORM FOLLOWUP OBSERVATIONS WITH JWST AND GROUND-BASED INSTRUMENTS AID THE INTERPRETATION OF TRANSIT AND ECLIPSE SPECTRA AND PROVIDE A BETTER UNDERSTANDING OF VOLATILE LOSS IN THESE ATMOSPHERES. SUCH RESULTS WILL HELP REFINE OUR PICTURE OF ROCKY PLANET FORMATION AND EVOLUTION. PLANETS IN ULTRA-SHORT PERIOD (USP) ORBITS ARE A SPECIAL CLASS OF HOT ROCKY EXOPLANETS. AS SHOWN BY KEPLER THESE PLANETS ARE GENERALLY SMALLER THAN 2 EARTH RADII SUGGESTING THAT THEY ARE LIKELY TO BE ROCKY AND COULD HAVE LOST THEIR VOLATILES THROUGH PHOTO-EVAPORATION. BEING CLOSE TO THEIR HOST STARS THESE PLANETS ARE ULTRA-HOT WITH ESTIMATED TEMPERATURES OF 1000-3000 K. A NUMBER OF USP PLANETS HAVE BEEN ALREADY DISCOVERED (E.G. KEPLER-78 B COROT-7 B KEPLER-10 B) AND THIS NUMBER IS EXPECTED TO GROW BY ING ADDITIONAL PLANET CANDIDATES. THE CHARACTERIZATION OF PLANETS ON ULTRA-SHORT ORBITS IS ADVANTAGEOUS DUE TO THE LARGER NUMBER OF OBSERVABLE TRANSITS AND THE LARGER TRANSIT SIGNAL IN THE CASE OF AN EVAPORATING ATMOSPHERE. MUCH ADVANCE HAS BEEN MADE IN UNDERSTANDING AND CHARACTERIZING HOT JUPITERS IN SIMILAR TRANSIT CONFIGURATIONS. FOR EXAMPLE NA HAS BEEN THE FIRST SPECIES TO BE DETECTED IN AN EXOPLANET ATMOSPHERE BY OBSERVING THE EVAPORATING HOT-JUPITER HD209458B. UNDERSTANDING THE INTERPLAY BETWEEN THE MAGMA OUTGASSING AND VOLATILE LOSS WILL BE AN IMPORTANT PART OF THIS PROJECT. OUR TEAM HAS THE EXPERTISE IN THE CHEMISTRY RADIATIVE TRANSFER AND ATMOSPHERIC ESCAPE MODELING AT THESE EXOTIC TEMPERATURES. OUR RECENT WORK HAS ANALYZED THE EMERGING ATMOSPHERES OF TERRESTRIAL PLANETS AFTER GIANT IMPACTS USING A WELL-ESTABLISHED RADIATIVECONVECTIVE ATMOSPHERIC STRUCTURE CODE WITH AN EXTENSIVE OPACITY DATABASE FOR ALL RELEVANT MOLECULES AND THE CHEMISTRY SELF-CONSISTENTLY CALCULATED FOR CONTINENTAL CRUST AND BULK SILICATE EARTH COMPOSITIONS. WE WILL EXPAND ON THIS WORK BY CONSIDERING A WIDER RANGE OF CHEMICAL COMPOSITIONS ASSESSING THE IMPORTANCE OF CLOUDS AND GENERATING CLOUDY MODELS AND DEVELOPING DIS-EQUILIBRIUM MODELS BY TAKING INTO ACCOUNT VERTICAL MIXING AND PHOTOCHEMISTRY. PHOTO-EVAPORATION WILL BE CONSIDERED IN THE ENERGY BALANCE BETWEEN HEATING COOLING AND MASS LOSS. WE ALSO HAVE IN-HOUSE CODES TO GENERATE HIGH-RESOLUTION ECLIPSE SPECTRA AND PREDICT TRANSIT DEPTHS AND OBSERVABLE SIGNATURES. THE DEVELOPMENT OF THE ATMOSPHERIC CODE THE MOLECULAR OPACITY UPDATES THE ATMOSPHERIC STRUCTURE CALCULATIONS AND THE HIGH RESOLUTION ECLIPSE SPECTRA WILL BE PERFORMED BY R. LUPU M. MARLEY AND R. FREEDMAN AT NASA AMES. THE ATMOSPHERIC CHEMISTRY GRIDS WILL BE PROVIDED BY B. FEGLEY AND K. LODDERS AT WASHINGTON UNIVERSITY. THE TRANSIT SPECTRA AND OBSERVATIONAL FEATURES WILL BE COMPUTED BY J. FORTNEY AT UCSC AND THE ATMOSPHERIC ESCAPE CALCULATIONS WILL BE PERFORMED BY K. ZAHNLE AT NASA AMES. THIS PROPOSAL ADDRESSES THE FOLLOWING GOALS OF THE EXOPLANET RESEARCH PROGRAM: EXPLAIN OBSERVATIONS OF EXOPLANETARY SYSTEMS AND UNDERSTAND THE CHEMICAL AND PHYSICAL PROCESSES OF EXOPLANETS. OUR RESULTS WILL ALSO INFORM FUTURE JWST OBSERVATIONS. $0 1/13/21 8 WE PROPOSE TO BUILD A VERSATILE SET OF SELF-CONSISTENT ATMOSPHERIC MODELS FOR HOT ROCKY EXOPLANETS AND USE THEM TO PREDICT THEIR TRANSIT AND ECLIPSE SPECTRA. HOT ROCKY EXOPLANETS WILL FORM THE MAJORITY OF SMALL PLANETS IN CLOSE-IN ORBITS TO BE DISCOVERED BY THE TESS AND KEPLER K2 MISSIONS, AND OFFER THE BEST OPPORTUNITY FOR CHARACTERIZATION WITH CURRENT AND FUTURE INSTRUMENTS. WE WILL USE FULLY NONGREY RADIATIVE-CONVECTIVE ATMOSPHERIC STRUCTURE CODES WITH CLOUD FORMATION AND VERTICAL MIXING, COMBINED WITH A SELF-CONSISTENT TREATMENT OF GAS CHEMISTRY ABOVE THE MAGMA OCEAN. BEING IN EQUILIBRIUM WITH THE SURFACE, THE VAPORIZED ROCK MATERIAL CAN BE A GOOD TRACER OF THE BULK COMPOSITION OF THE PLANET. WE WILL DERIVE THE ATMOSPHERIC STRUCTURE AND ESCAPE RATES CONSIDERING BOTH VOLATILEFREE AND VOLATILE BEARING COMPOSITIONS, WHICH REFLECT THE DIVERSITY OF HOT ROCKY PLANET ATMOSPHERES. OUR MODELS WILL INFORM FOLLOWUP OBSERVATIONS WITH JWST AND GROUND-BASED INSTRUMENTS, AID THE INTERPRETATION OF TRANSIT AND ECLIPSE SPECTRA, AND PROVIDE A BETTER UNDERSTANDING OF VOLATILE LOSS IN THESE ATMOSPHERES. SUCH RESULTS WILL HELP REFINE OUR PICTURE OF ROCKY PLANET FORMATION AND EVOLUTION. PLANETS IN ULTRA-SHORT PERIOD (USP) ORBITS ARE A SPECIAL CLASS OF HOT ROCKY EXOPLANETS. AS SHOWN BY KEPLER, THESE PLANETS ARE GENERALLY SMALLER THAN 2 EARTH RADII, SUGGESTING THAT THEY ARE LIKELY TO BE ROCKY AND COULD HAVE LOST THEIR VOLATILES THROUGH PHOTO-EVAPORATION. BEING CLOSE TO THEIR HOST STARS, THESE PLANETS ARE ULTRA-HOT, WITH ESTIMATED TEMPERATURES OF 1000-3000 K. A NUMBER OF USP PLANETS HAVE BEEN ALREADY DISCOVERED (E.G. KEPLER-78 B, COROT-7 B, KEPLER-10 B), AND THIS NUMBER IS EXPECTED TO GROW BY ING ADDITIONAL PLANET CANDIDATES. THE CHARACTERIZATION OF PLANETS ON ULTRA-SHORT ORBITS IS ADVANTAGEOUS DUE TO THE LARGER NUMBER OF OBSERVABLE TRANSITS, AND THE LARGER TRANSIT SIGNAL IN THE CASE OF AN EVAPORATING ATMOSPHERE. MUCH ADVANCE HAS BEEN MADE IN UNDERSTANDING AND CHARACTERIZING HOT JUPITERS IN SIMILAR TRANSIT CONFIGURATIONS. FOR EXAMPLE, NA HAS BEEN THE FIRST SPECIES TO BE DETECTED IN AN EXOPLANET ATMOSPHERE, BY OBSERVING THE EVAPORATING HOT-JUPITER HD209458B. UNDERSTANDING THE INTERPLAY BETWEEN THE MAGMA OUTGASSING AND VOLATILE LOSS WILL BE AN IMPORTANT PART OF THIS PROJECT. OUR TEAM HAS THE EXPERTISE IN THE CHEMISTRY, RADIATIVE TRANSFER, AND ATMOSPHERIC ESCAPE MODELING AT THESE EXOTIC TEMPERATURES. OUR RECENT WORK HAS ANALYZED THE EMERGING ATMOSPHERES OF TERRESTRIAL PLANETS AFTER GIANT IMPACTS, USING A WELL-ESTABLISHED RADIATIVECONVECTIVE ATMOSPHERIC STRUCTURE CODE, WITH AN EXTENSIVE OPACITY DATABASE FOR ALL RELEVANT MOLECULES, AND THE CHEMISTRY SELF-CONSISTENTLY CALCULATED FOR CONTINENTAL CRUST AND BULK SILICATE EARTH COMPOSITIONS. WE WILL EXPAND ON THIS WORK BY CONSIDERING A WIDER RANGE OF CHEMICAL COMPOSITIONS, ASSESSING THE IMPORTANCE OF CLOUDS AND GENERATING CLOUDY MODELS, AND DEVELOPING DIS-EQUILIBRIUM MODELS BY TAKING INTO ACCOUNT VERTICAL MIXING AND PHOTOCHEMISTRY. PHOTO-EVAPORATION WILL BE CONSIDERED IN THE ENERGY BALANCE BETWEEN HEATING, COOLING AND MASS LOSS. WE ALSO HAVE IN-HOUSE CODES TO GENERATE HIGH-RESOLUTION ECLIPSE SPECTRA AND PREDICT TRANSIT DEPTHS AND OBSERVABLE SIGNATURES. THE DEVELOPMENT OF THE ATMOSPHERIC CODE, THE MOLECULAR OPACITY UPDATES, THE ATMOSPHERIC STRUCTURE CALCULATIONS AND THE HIGH RESOLUTION ECLIPSE SPECTRA WILL BE PERFORMED BY R. LUPU, M. MARLEY, AND R. FREEDMAN AT NASA AMES. THE ATMOSPHERIC CHEMISTRY GRIDS WILL BE PROVIDED BY B. FEGLEY AND K. LODDERS AT WASHINGTON UNIVERSITY. THE TRANSIT SPECTRA AND OBSERVATIONAL FEATURES WILL BE COMPUTED BY J. FORTNEY AT UCSC, AND THE ATMOSPHERIC ESCAPE CALCULATIONS WILL BE PERFORMED BY K. ZAHNLE AT NASA AMES. THIS PROPOSAL ADDRESSES THE FOLLOWING GOALS OF THE EXOPLANET RESEARCH PROGRAM: EXPLAIN OBSERVATIONS OF EXOPLANETARY SYSTEMS, AND UNDERSTAND THE CHEMICAL AND PHYSICAL PROCESSES OF EXOPLANETS. OUR RESULTS WILL ALSO INFORM FUTURE JWST OBSERVATIONS. Other Administrative Action $0 1/22/20