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• W1618984761 abstract "The research focused on molecular hydrogen and its response to ultraviolet radiation, photoelectron impact excitation and X-ray radiation and on interpretation of ultraviolet spectra of Jupiter dayglow and auroras. A systematic effort was made to obtain reliable rate coefficients for rovibrational energy transfer of H2, particularly in collisions with hydrogen atoms. We carried out elaborate quantum-mechanical calculations of scattering of H and H2 on what had been characterized as a reliable potential energy surface of H3 molecular system. These calculations took into account reactive channels and rate coefficients for ortho-para transitions were obtained. Quantal calculations are too complex to be applied to all possible rovibrational transitions and we turned to a semi-classical method. With it we calculated rate coefficients for transitions, reactive and non-reactive, for all rovibrational levels. We carried out calculations for three of available H3 potential energy surfaces. We discovered an unexpected sensitivity of rate coefficients for non-reactive channels to potential energy surface. This discovery stimulated more thorough investigations of potential energy surface elsewhere and to construction of a new surface. We have used it in further semi-classical calculations in work that will shortly be 2 completed and which, together with new quantum-mechanical calculations should comprise a set of reliable rate coefficients that can be used in discussions of H2 on Jovian planets. We carried out a detailed study of Jovian ultraviolet dayglow. There has been a long-running argument about dayglow on Jupiter. There are two sources of excitation: fluorescence and photoelectron impact excitation. It had been argued that a third source the electron glow was needed to bring theory and observation into agreement. We believe we have shown conclusively that third source is unnecessary. We have achieved a close quantitative agreement between predicted spectrum arising from fluorescence and photoelectrons and measured spectrum. We also demonstrated a method by which presence of HD could be established observationary. Similar calculations were carried out of ultraviolet spectra of Jovian auroras. We again found close agreement. Indeed, agreement was so detailed we were able to derive temperature of atmosphere. We found, contrary to standard model of time, a high temperature between 400 K and 600 K and established presence of a significant temperature gradient. A large temperature gradient was indeed found by direct sampling with Jupiter probe." @default.
• W1618984761 created "2016-06-24" @default.
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• W1618984761 date "1993-04-01" @default.
• W1618984761 modified "2023-09-23" @default.
• W1618984761 title "Molecular processes in comets" @default.
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