Ion Chemistry in Atmospheric and Astrophysical Plasmas

Details Ion Chemistry in Atmospheric and Astrophysical Plasmas Ion Chemistry in Atmospheric and Astrophysical Plasmas

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994stin...9623210d&link_type=abstract

Journal Article, Harvard-Smithsonian Center for Astrophysics Cambridge, MA United States

Astronomy and Astrophysics

Astrophysics

Ionic Reactions, Atmospheric Chemistry, Chemical Reactions, Cosmic Gases, Cosmic Rays, Interstellar Matter, Molecular Clouds, Planetary Atmospheres, Planetary Ionospheres, Star Formation, Ultraviolet Radiation, Background Radiation, Combustion, Electron Impact, Gamma Rays, Gas Giant Planets, Gravitational Collapse, Heavy Elements, Helium Ions, Ionized Gases, Radiation Distribution, Space Plasmas, Stellar Envelopes, Supernovae, Titan, Uniform Flow

Scientific paper

There are many differences and also remarkable similarities between the ion chemistry and physics of planetary ionospheres and the ion chemistry and physics of astronomical environments beyond the solar system. In the early Universe, an expanded cooling gas of hydrogen and helium was embedded in the cosmic background radiation field and ionized by it. As the Universe cooled by adiabatic expansion, recombination occurred and molecular formation was driven by catalytic reactions involving the relict electrons and protons. Similar chemical processes are effective in the ionized zones of gaseous and planetary nebulae and in stellar winds where the ionization is due to radiation from the central stars, in the envelopes of supernovae where the ionization is initiated by the deposition of gamma-rays, in dissociative shocks where the ionization arises from electron impacts in a hot gas and in quasar broad-line region clouds where the quasar is responsible for the ionization. At high altitudes in the atmospheres of the Jovian planets, the main constituents are hydrogen and helium and the ion chemistry and physics is determined by the same processes, the source of the ionization being solar ultraviolet radiation and cosmic rays. After the collapse of the first distinct astronomical entities to emerge from the uniform flow, heavy elements were created by nuclear burning in the cores of the collapsed objects and distributed throughout the Universe by winds and explosions. The chemistry and physics became more complicated. Over 90 distinct molecular species have been identified in interstellar clouds where they are ionized globally by cosmic ray impacts and locally by radiation and shocks associated with star formation and evolution. Complex molecules have also been found in circumstellar shells of evolved stars. At intermediate and low altitudes in the Jovian atmospheres, the ion chemistry is complicated by the increasing abundance of heavy elements such as carbon, and an extensive array of complex molecules has been predicted. Reactions involving heavy elements dominate the structure of the ionspheres of the terrestrial planets and the satellites Titan and Triton.

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