Even four

Text:
Results
-Ion production and direct heating - needs results
-Chemistry (further)? - needs coding
-Heating (further - Joule heating etc)? - needs coding
-Photons - needs results
-Sensitivities - needs results
Discussion - needs results
Conclusions - needs results

Figures:
4.6 - Validation monoruns - runs ongoing
4.13 - Uranus North ion production - ongoing
4.14 - Uranus South ion production - ongoing
4.16 - Uranus heating - ongoing
4.19 - Peak rate altitudes, Uranus - needs runs
4.24 - H3+ densities for three cases Saturn(?) - needs coding, runs
4.25 - H3+ densities for three cases Uranus(?) - needs coding, runs
4.26-8 - Sensitivity graphs for Saturn, three whole 3D graphs - runs ongoing

Tables:
4.2 - Ion production Uranus - runs ongoing
4.4 - Heating Uranus - runs ongoing
4.5 - H3+ Saturn(?) - needs coding, runs
4.6 - H3+ Uranus(?) - needs coding, runs

Modelling required:
Validation runs (three cases - highly intensive due to powerful aurora) - ongoing
Uranus runs (two cases - very low intensity aurora) - ongoing
Chemistry module - coding to update for certain Steve based things, then runs using model atmospheres and ion production
Sensitivities - you can't miss these runs, they've been going for a year now... - ongoing

Two bits of coding remain as well as loads of calculations etc. Once these two are done and set off, I can start reformatting graphs on the paper version. I have two to compress and one to create, which depends on one of the set of runs listed here...

More questions from BAS... sigh. If they'd only wait a couple of days, I'll be on Chapter five anyway...

Testrun numbers calculated for Grodent cases (ok, updated...). All cases running (all four that is, as one extra has crept in). This means keter now has Uranus, Validation and Sensitivities runs going. C3 has alpha runs, except one that rimmer has.

Soooo. Chemistry. Chemical rates are heirarchical, which means you must get the major species right before thinking about the minor species, else you'll be iterating massively forever. H2 is the most major species, followed by He and then H (neutrals). The largest charged species is e-, followed initially by H2+, later to become H3+, then He+ and H+. I could go further, inlude hydrocarbons, He++ etc, but for the initial check not necessary - though Steve wants rotational level chemistry, which means sticking in all 27 levels of H3+ seperately and letting them decay into appropriate populations...

I have devised simple balance equations, using the production, loss and initial density terms for each thing. Next will be to iterate over and again until this lot reach new densities. Highest danger will be to the photoionisation rates at the top, which will mean considerable ionisation of some low density species, low densities fluctuate, hence so will the photoionisation rates. Similar considerations are required for auroral ionisation later... The reason for using this order isn't just because the big things changing changes the little things so much, but also because the little things change the big things so little...

But first, bits and pieces of graphs. Ok, after battles with p!multi, extra y-axes, positioning things etc, I finally have two graphs in one eps with both pressure and altitude scales attached. The other graphs are less essential. Or perhaps I'm lazy, either way they won't get 'em. Have adjusted captions and official review response. There now really is only one thing to do - the validations, which are cooking on Keter as we speak.