. "Astrochemistry"@en . . "3" . "The space between the stars is not empty but filled with a very dilute gas with extremely low densities and temperatures, providing a unique laboratory with conditions not normally encountered on Earth. A surprisingly rich chemistry occurs in these so-called interstellar clouds, as evidenced by the discovery of more than 200 different molecules. Some of these species were found in space before they were identified in a laboratory on Earth. How are these molecules formed? Where are they found and how do astronomers identify them? How do their abundances differ from place to place and what does this tell us about the structure of the region? How do the abundances evolve from cold clouds to planet-forming disks, where they can form the basis for prebiotic species?\n\nThe outline of the course is as follows:\n\nBasic principles of gas-phase and gas-grain chemical reactions\nChemistry in the early Universe\nChemistry in diffuse and translucent clouds, and in photon-dominated regions\nChemistry in shocks\nEvolution of molecular abundances from dark pre-stellar cores to star-forming regions\nChemistry in protoplanetary disks and links with comets\n\nOutcome:\nThe student will gain relevant background information that will enable him/her to follow the current literature on Astrochemistry and to do research in this field. The student will also acquire hands-on experience with running molecular excitation and chemical network codes, and make predictions for ALMA." . . "Presential"@en . "TRUE" . . "Astrochemistry"@en . . "3" . "The space between the stars is not empty but filled with a very dilute gas with extremely low densities and temperatures, providing a unique laboratory with conditions not normally encountered on Earth. A surprisingly rich chemistry occurs in these so-called interstellar clouds, as evidenced by the discovery of more than 200 different molecules. Some of these species were found in space before they were identified in a laboratory on Earth. How are these molecules formed? Where are they found and how do astronomers identify them? How do their abundances differ from place to place and what does this tell us about the structure of the region? How do the abundances evolve from cold clouds to planet-forming disks, where they can form the basis for prebiotic species?\r\n\r\nThe outline of the course is as follows:\r\n\r\nBasic principles of gas-phase and gas-grain chemical reactions\r\n\r\nChemistry in the early Universe\r\n\r\nChemistry in diffuse and translucent clouds, and in photon-dominated regions\r\n\r\nChemistry in shocks\r\n\r\nEvolution of molecular abundances from dark pre-stellar cores to star-forming regions\r\n\r\nChemistry in protoplanetary disks and links with comets\n\nOutcome:\nThe student will gain relevant background information that will enable him/her to follow the current literature on Astrochemistry and to do research in this field. The student will also acquire hands-on experience with running molecular excitation and chemical network codes, and make predictions for ALMA." . . "Presential"@en . "TRUE" . . "astrochemistry and astrobiology"@en . . "3" . "Astrochemistry (15h) 1) Historical roots of astrochemistry. 2) Production of chemical elements in stars. 3) The Big Bang nucleosynthesis - first atoms. 4) Molecular complexity - \"bottom-up\" and \"top-down\" approaches. Organic mole$ 5) Processes on dust grains. Astrobiology (15h) - formation and evolution of planetary systems - physicochemical conditions on the planets and moons of the Solar System - emergence and evolution of life - rocky exoplanets and exomoons in circumstellar habitable zones - the Drake equation, methods of searching for extraterrestrial intelligence" . . "Presential"@en . "FALSE" . . "Astrochemistry"@en . . . . .