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Publication Detail
H-3(+) cooling in planetary atmospheres
  • Publication Type:
    Conference
  • Authors:
    Miller S, Stallard T, Melin H, Tennyson J
  • Publisher:
    ROYAL SOC CHEMISTRY
  • Publication date:
    2010
  • Pagination:
    283, 291
  • Published proceedings:
    FARADAY DISCUSSIONS
  • Volume:
    147
  • Name of conference:
    Conference on Chemistry of the Planets
  • Conference place:
    Brittany, FRANCE
  • Conference start date:
    14/06/2010
  • Conference finish date:
    16/06/2010
  • Print ISSN:
    1364-5498
  • Language:
    EN
  • Keywords:
    1ST PRINCIPLES CALCULATIONS, JOVIAN UPPER-ATMOSPHERE, ROVIBRATIONAL TRANSITIONS, JUPITERS THERMOSPHERE, THERMAL BALANCE, PRIMORDIAL GAS, GRAVITY-WAVES, IONOSPHERE, H-3+, EVOLUTION
  • Addresses:
    Miller, S
    UCL
    Dept Phys & Astron
    London
    WC1E 6BT
    England
Abstract
We review the role of H-3(+) in planetary atmospheres, with a particular emphasis on its effect in cooling and stabilising, an effect that has been termed the "H-3(+) thermostat'' (see Miller et al., Philos. Trans. R. Soc. London, Ser. A, 2000, 58, 2485). In the course of our analysis of this effect, we found that cooling functions that make use of the partition function, Q(T) based on the calculated H-3(+) energy levels of Neale and Tennyson (Astrophys. J., 1995, 454, L169) may underestimate just how much energy this ion is radiating to space. So we present a new fit to the calculated values of Q(T) that is accurate to within 2% for the range 100 K to 10 000 K, a very significant improvement on the fit originally provided by Neale and Tennyson themselves. We also present a fit to Q(T) calculated from only those values Neale and Tennyson computed from first principles, which may be more appropriate for planetary scientists wishing to calculate the amount of atmospheric cooling from the H-3(+) ion.
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