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Correcting the small increments thing in the Jupiter model. It is in there, but not recorded, bizzarely enough.

Subroutines to alter:
electron - checked, declared, changed - done!
strike - checked, declared, changed - done!
proton - declarations - done!
proton1 - declarations - done!
hit - checked against Earth model, changed declarations, changed recording - done!
back - checked, declared, changed - done!
selectron - checked, declared, changed - done!
recoil - checked, declared, changed - done!

All done.

Compiled.

Running.

Why did I do that? All the hard work had been done, just hadn't redeclared the results arrays as real variables, instead leaving them as integers. Makes it easier to analyse, I suppose, but artificially inflates results in denser or energy degraded areas. I know this has little effect in Gas Giant atmospheres and I may have removed it to reduce computational time and keep things looking pretty, but the calculations were left in, so no time was reduced and things won't look pretty if they're recording incorrectly...

Ok, results are in. That's better. Enough of this madness, at last. Shape is looking good, peak position great, magnitude very good.

More of the same

Chapter four:
1,193 -> 2,950

A quick one, but nevertheless full. I have extended the paper to include all the bits cut out to fit the thing in the GRL format. Although this is the shortest chapter, it is probably the most complete as I doubt Alan will cut it up as much as the rest. I will be including a few extra graphs and tables, which means the captions and bodies will increase the word count. Not too much, but enough.

One graph, of course, remains undone - the Grodent one. As the Thesis is almost up to speed, this can be started... and when I say almost, I think I could do a paragraph on Jupiter... may as well.

Chapter six:
0 -> 888

Total:
25,432 -> 28,077
46.795%

I guess that's about it for the writing at the moment. Though I can put extra bits in, they would be slow and really dependant on the results that go in there - which is the thing to work on next.

First, a restatement of how things stand:

Introduction:
5,549
Chapter 2:
7,512
Chapter 3:
7,173
Chapter 4:
2,950
Chapter 5:
3,995
Chapter 6:
888

I will need to move sensitivities from Chapter three back to chapter 4 to balance them. May also shift the Jovian validation too... Maybe even the terrestrial one... just leave protons and photons in three. Photons (investigation into the effect of scattering, plus Chapman function and validation) could go into Chapter six too. At least I'll cool the ardour of Chapter three (plus make it easier to complete).

ok, have started on further interpolation of the Grodent atmosphere...

Continuing

Ok, on with the checks:

1.38 KeV
100k

2.03 KeV
1M+ (Hurray!)

2.98 KeV
1M

4.4 KeV
1M+ (Hurray!)

6.4 KeV
10,000ok

9.4 KeV
1000ok

14 KeV
1000ok

20.8 KeV
1000ok

30.5 KeV
1000ok

...where 'ok' is listed it means the energy has been checked at that flux, but no higher yet. Higher energy electrons take longer to deal with as they pass through a larger slab of atmosphere, they penetrate into the small increments area requiring extra calculations, they last longer and they produce more secondaries that require thermalisation. Fortunately, above a certain energy, they're also able to fly through the atmosphere with few interactions. Unfortunately, we're not dealing with those energies...

There is a problem to be resolved to do with excitation recording, which mismatches altitudes and array size. This will be sorted. It is done. I'll compile at a later date - the program will, that is, not me myself.

Have grabbed even more profiles off Makenzie.

More work

Brief overview with the 'new era of Jovian auroral understanding' ie Steve's ideas on Makenzie's profiles. Yep, there are new ones, lots of them, with interesting things to look at.

One run finished (the last of the set that were running, meaning all I have to do is wait until the new regime is in place and set off the seven old ones again). Saturn5000 was the 12eV SD+1 run. It has been analysed.

Of course, first there is CTIP...

I have just had a look at putting the small increments thing in and it seems ok. Like everything else...

Sigh, "bus errror", should'a known it...

hmmm, will try a few runs on other computers using proton1...

Fails on rimmer

can't compile on C3

Going on keter... on the slow processors...

Trying out 31eV runs whilst waiting. It doesn't dip into the small increments level too deeply at this point, so may or may not avoid bus errors. On the other hand, ramping up the number of electrons fired does invite more errors to show their hand...

...bus error at 100k dammit!

Hmmm, difficult one. The lower energy stuff could probably quite happilly live without the small increments stuff, but the high energy stuff really needs it, otherwise there's the risk of crossing into an unrealistic pressure level. I'll run through the other energies and see if any of them can complete...

...one minor comfort, doing the 46eV lot, is that I do get ionisation in all pressure levels, as hoped.

...bus error at 100k

66eV
...100k again

96eV
...1M this time. Dammit... so close...

140eV
100k

206eV
100k

300eV
1M

440eV
1M

650eV
1M+ (hurray!)

950eV
1M

Don't yet have time to try out:
1380, 2030, 2980, 4400, 6400, 9400, 14000, 20800, 30500

I have actually remembered that since I have to divide all answers by a thousand to account for path length, 100k is more than enough anyway... and the answers (suggesting final peak rates from just shy of 1000 to just shy of 10,000 pcm3) is what is expected.

Must/may also do runs with pitch angle distributions, plus magnetic effects... after all...

Marking

Marking

Plus updated TIROS entry and had quick meeting with Steve about Makenzie's stuff.

More on x-rays

Well, photons. The Klein-Nisch formula gives compton (x-rays) and Thompson (lower energy than x-rays) cross-sections for scattering off electrons. Data can also be found for absorption, ionisation, dissociation, Rayleigh/Mie (visible scattering off dust) and Raman (absorption, plus re-emission at another wavelength). This is all photons do. Well, in my model it will be... Plus need to establish the effect of the Sun being an extended source, and see if I can get my photons to curve...

Need differential pdfs from each type of scattering plus total cross-sections.

One run has finished so far. 40eV completed its SD+2 run, was analysed, recoded and set off again without grade changes.

Ok, after a bit of research, it probably won't matter (ok, certainly won't matter) if I keep the backscatter ratio at 0.5 as that is what it is below about 0.2MeV (far more energetic than 1nm). There isn't anything to worry about so far as energy transfer after all, so just need to put compton scattering total cross-section (which I have) into the program as a normal, scattering (incoherent) cross-section. Then, absorption, dissociation and ionisation ones go in as normal. Rayleigh/Mie can't be used as there's no dust in the models, so that just leaves Raman, which has already been stuck in there. Thompson is implictly included through the Compton computation as mentioned above. Ok, I'm ready to rock...

Have scraped together a load of cross-sections for a 1nm grid of x-ray fluxes. Need a few molecular ones, but have compton ones, plus a few photoionisation and absorption ones for elements - enough, at least, to interpolate the rest from.

Have also had another cloudy day at Mill Hill. 100% cloud cover at least...

H3+ profile has come through from Makenzie.

More and more and more...

Another block of maths demonstrating out of the way.

One run has finished. Saturn1000 slot 100keV GS1m run. Analysis was as expected. Recoded as GS10 version of same energy and set off again. Have decided to kill off all the fast runs asap rather than do them concurrently with the slow runs, then do all the slow runs in one big block - asides from those currently being done and their heirs...

Not that any 'fast' runs are left asides fro the 100keV ones. All medium to slow.

Also had a quick look at Makenzie's newly produced profiles. She hasn't produced the further out ones, which are the important ones yet, so will wait until tomorrow for discussions. Or later. Who knows...

...one last thing. References for Martian cross-sections kept from Europlanet, this list I will be going through for obvious reasons:
Straub et al 1996 - already got
Lindsay et al 2000 - now got
Manyan et al 2000 - ah, ManGan et al... ahem, now got...
Deutsch et al 2002 - now got
Haider et al 1992 (modelling) - JGR, dammit!
Erdman and Zopt 1983 (cameron band?) - ZIPF, what sort of a name is that? Far prefer Zopt... Anyway, not included in UCL's subscription to Planetary and space science, so no-go despite importance...
Fox and Dalgarno 1979 - JGR - though did get hold of three 1979 papers by Dalgarno relating to proton processes I was in dire need of for DICE...
Lummerzhien and Lilensten 1994 - Lummerzheim, given I own half his back catalogue, it sometimes seems, I should know how to spell his name... plus annales has withdrawn the PDF! Did they know I wanted it?
Tran and Vidal 1998 - TIan... now got, oh!, there's another, got it too. Waaaaait. A third useful Tian and Vidal 1998 has appeared with cross-sections, my they had a busy year - nope, here's number four, maybe Tian and Vidal 1998 is a generic reference to their entire career...
Torr and Torr 1985 (Photon)
Avalgan et al 1998 (Photon)
Hitchcock et al 1980 (Photon)
Masuoka 1994 (Photon)

Will deal with the photon stuff another time. Mostly have them, but no real prospect of a photon thing to deal with yet as Tommi is otherwise engaged.

I make no garrentees that any of those names are spelt correctly, or in any way resemble the correct spellings.