Miller, S; Stallard, T; Melin, H; Tennyson, J; (2010) H-3(+) cooling in planetary atmospheres. In: FARADAY DISCUSSIONS. (pp. 283 - 291). ROYAL SOC CHEMISTRY
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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.
|Title:||H-3(+) cooling in planetary atmospheres|
|Event:||Conference on Chemistry of the Planets|
|Dates:||2010-06-14 - 2010-06-16|
|Keywords:||1ST PRINCIPLES CALCULATIONS, JOVIAN UPPER-ATMOSPHERE, ROVIBRATIONAL TRANSITIONS, JUPITERS THERMOSPHERE, THERMAL BALANCE, PRIMORDIAL GAS, GRAVITY-WAVES, IONOSPHERE, H-3+, EVOLUTION|
|UCL classification:||UCL > School of BEAMS > Faculty of Maths and Physical Sciences > Physics and Astronomy|
UCL > School of BEAMS > Faculty of Maths and Physical Sciences > Science and Technology Studies
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