THE RESEARCH PROJECT INCLUDES TWO ASPECTS: SPACE TECHNOLOGY AND SCIENCE. AFTER HAVING DESIGNED THE POWER CONVERTER MODULES FOR THE JANUS AND GALA INSTRUMENTS OF THE JUICE MISSION, AS WELL AS THE FILTER WHEEL MODULE FOR THE CAMERA JANUS, WE ENTER THE PHASE OF DELIVERING THE FLIGHT MODELS TO THE TWO INSTRUMENT CONSORTIA, AND THEN TO ESA. BOTH INSTRUMENTS ARE WITHIN THE SCIENTIFIC PAYLOAD OF JUICE MISSION (ESA) TO JUPITER AND ITS SYSTEM._x000D_ THE SCIENTIFIC SIDE IS ORIENTED TO THE CONTINUATION OF THE SCIENTIFIC EXPLOITATION OF THE DATA FROM THE OSIRIS CAMERA ABOARD THE ROSETTA SPACECRAFT (ESA MISSION TO COMET 67P/CHURYUMOV- GERASIMENKO) IN THE FRAME OF THE DISCOVERIES OF OTHER INSTRUMENTS DATA. SEVERAL OPEN QUESTIONS STILL REMAIN AS THE ORIGIN AND FORMATION OF THE COMETARY NUCLEII. DATA FROM THE ROSETTA MISSION AS WHOLE PUT INTO DOUBT THE WIDELY ACCEPTED IDEA OF A COLLISIONAL OUTER SOLAR SYSTEM. THE IN DEPTH STUDY OF THE EVOLUTION OF THE ROTATIONAL STATE OF THE NUCLEUS CAN SHED LIGHT ON THE INTERNAL STRUCTURE OF THE NUCLEUS, AND THUS ON ITS COLLISIONAL HISTORY. FOR THIS, WE WILL PERFORM SIMULATIONS IN ORDER TO REPRODUCE THE 67P GAS PRODUCTION RATE. THE CODE DEALING WITH ROTATIONAL EVOLUTION MUST INCLUDE (I)MORE VOLATILE SPECIES (CO, CO2), (II)THE IMPULSE PRODUCED BY OUTBURSTS, AND (III)THE ROLE OF ROTATIONAL EXCITATION IN ROTATIONAL EVOLUTION._x000D_ IT IS OUR PLAN TO CONTINUE THE STUDY OF THE COMPOSITION OF THE REDUCING ATMOSPHERES OF THE ICY GIANT PLANETS (AS URANUS AND NEPTUNE). WE PLAN TO FOCUS ON URANUS WHERE RECENTLY CO HAS BEEN DISCOVERED IN ITS STRATOSPHERE. THE DISCOVERY IS SUCH THAT WE CANNOT ASCERTAIN THE ORIGIN OF THE MEASURED. THE MEASURED ABUNDANCE CAN BE REPRODUCED WHEN MODELING THREE DIFFERENT SCENARIOS: A SUDDEN EVENT AS A COMETARY IMPACT DELIVERING CO, A STEADY SOURCE AS THE ONE DUE TO ICY GRAINS ABLATION, AND A COMBINATION OF BOTH. THE CONCENTRATION OF THE OTHER OXYGEN SPECIES DETECTED IN THIS ATMOSPHERE (H2O BY ISO) AND CO2 (BY SPITZER) DO NOT HELP TO DISCRIMINATE AMONG THE THREE SCENARIOS OUTLINED. OUR MODELS, RECENTLY PUBLISHED CAN ONLY CONFIRM THAT WATER NEEDS TO BE SUPPLIED TO THIS PLANET BY A STEADY SOURCE, BUT CO AND CO2 CAN HAVE A DUAL ORIGIN. ONE WAY TO SOLVE THIS DILEMMA IS TO DETECT OTHER SPECIES PRESENT IN THE COMET AND DEPOSITED IN THE ATMOSPHERE AFTER THE COLLISION. HYDROGEN CYANIDE IS A GOOD CANDIDATE AND IT CAN BE ALSO DETECTED BY ALMA (PROVIDED THAT THE MIXING RATIO IS LARGER THAN 1E-13 IN THE STRATOSPHERE). THEREFORE, WE PLAN TO EXTEND OUR URANUS PHOTOCHEMICAL MODEL TO NITROGEN CHEMISTRY BUILDING A C-N-O CHEMICAL NETWORK THAT, ON ONE HAND, CAN MODEL THE EXISTENCE OF HCN DUE TO AN INTERNAL SOURCE OF N2 (WHICH IS DISSOCIATED BY GALACTIC COSMIC RAYS IMPACT AND THEN REACT WITH CH4 PHOTOLYSIS PRODUCTS) AND/OR DUE TO A COMETARY IMPACT. SHOULD ALMA DETECT CARBON MONOXIDE AND HYDROGEN CYANIDE, THE ABUNDANCE (AND THE VERTICAL MIXING RATIO PROFILES) WILL UNDOUBTEDLY DETERMINE THE ORIGIN NOT ONLY OF HCN BUT ALSO OF CO. HERE THE CHALLENGE IS TO DETERMINE THE PRIMORDIAL N2 EXISTING IN THE VERY DEEP ATMOSPHERE. FOR THIS, OUR THERMOCHEMICAL MODELS DEVELOPED FOR EXOPLANETARY ATMOSPHERES COMPOSITION WILL BE APPLIED. _x000D_ EXOPLANETARY ATMOSPHERIC OBSERVATIONS CANNOT BE ACCURATELY INTERPRETED TO DATE. THE ROLE THAT AEROSOLS PLAY ON THIS ATMOSPHERES IS NOT COMPLETELY UNDERSTOOD AND POINT TO BE ONE OF THE MAIN CAUSES. IN THIS PROJECT, WE WILL TRY TO UNDERSTAND HOW AEROSOLS CAN AFFECT THE ATMOSPHERIC GASEOUS COMPOSITION.