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.

Back to CTIP-type

Ok, still need to adjust the NDenses:
electron - common blocks, declarations, pdf, adjustments, selection - done!
strike - common blocks, declarations, pdf, adjustments, selection - done!
proton - common blocks, declarations, files, arrays, outputs - done!
proton1 - common blocks, declarations, files, arrays, outputs - done!
selectron - common blocks, declarations, pdf, adjustments, selection - done!
recoil - common blocks, declarations, pdf, adjustments, selection - done!
back - common blocks, declarations, pdf, adjustments, selection - done!
hit - common blocks, declarations, pdf, adjustments, selection - done!

But does it all compile? Yep.

Now I have a model with O, O2 and N2 being struck by incoming electrons, with no magnetic effects, as desired. However, this model contains old MSIS number densities. To convert to CTIP type completely, I need the CTIP densities in there as well as the altitude range.

The list of subroutines is:
randgen - no change
atom - no change
cross - no change
electron - changes
strike - changes
proton - changes
proton1 - changes
selectron - changes
recoil - changes
back - changes
hit - changes

Curent state of the input files:
NDens0 - Changes
NDens1 - Changes
NDens2 - Changes
NDens3 - Changes
Temp - Changes

...although I fear I may require one or two other pressure levels for expansion... we shall see...

ok, lets 'ave a look.

We're going from 1-600km to 80-580km, a change from 600 to 501 altitude levels.

Ok, changes in input files:
NDens0 - number of levels altered
NDens1 - CTIP numbers in
NDens2 - CTIP numbers in
NDens3 - CTIP numbers in
Temp - CTIP numbers in

Easy to follow...

So, subroutines:
electron - declarations, altitude incrementation, recording - done!
strike - declarations, alt. inc., recording - done!
proton - declarations, orientation adjustment, output - done!
proton1 - declarations, orientation adjustment, output - done!
selectron - declarations, alt. inc., recording - done!
recoil - declarations, alt. inc., recording - done!
back - declarations, alt. inc., recording - done!
hit - declarations, alt. inc., recording - done!

Compilation stuff - compiled first time

suspicious...

Quick test. 1keV gives 100+ km peak, sounds fine.

Another quick test. 10keV gives peak around 90km.

Yet another quick test. 30keV gives peak above 80km.

Seems ok so far.

100eV peaked - if that's the word - at about 130km. 50eV above it.

All the alts should be a little low as its a winter solstice atmosphere. They are indeed a little low, but not by too much in comparison to the atmospheric motion (we've lost about 20km cf the msis density height). Hmmm. Seems to work. For the really high energy stuff, I should add a lower atmospheric bin that can take the additional levels of precipitation and hold them for later uses (ie, total number of ionisations/excitations etc should remain equal as the atmosphere expands/contracts etc). Of course, further reasons for them being lower include the lack of mirroring or any pitch angle effects in there, plus no tilted field lines, as would be normal. Yep, a quick run raises the 1keV peak by nearly 10km when including the tilt. A pa spectru shouldn't be as significent a raise, but including mirroring and expansion, I think it's a pretty safe bet that the model's ok.

So, now I have a 'working' model, I can ruin it. I mean, use it. I need to feed through about a million electrons of each of the 19 DMSP levels. For the upper energies, this can be done immediately as they'll thermalise in the atmosphere above the lower boundary. For the high energy stuff, I'll need a lower atmosphere to help ascertain how much total ionisation there is - and the energy expended in creating it. Usefull here is the secondary/primary split, which tells me what the primary beam is doing and what the secondary beam then does. Changes in the primary beam affect the secondary beam - this is of paramount importance in the really high energy stuff. Not sure I'll actually use it here though...

We require:
31, 46, 66, 96, 140, 206, 300, 440, 650, 950, 1380, 2030, 2980, 4400, 6400, 9400, 14000, 20800, 30500eV runs.

Hmmm, should validate this thing soon... beyond the wishy washy validations and the validations of other near identical models. This one's new and has a defined purpose... plus it predates the arrival of the protonic version that should seal my fate...

It is total energy flux devoted to ionisation that needs to be conserved, so, in effect, it doesn't matter what the lower atmospheric composition is, just how many wallops I get from it... and from what in it... (in the case of those electrons of low enough energy to care).

Now, asides from anything else, I need to plot out what should happen for the proton version. I require:
O, O+, O-, O2, O2+, O2-, N2, N2+, N2-, H, H+, H-, e-
...and a grid of cross-sections between each of them and themselves, each one equivalent to the size of the e- grid.

Frightening innit. And that's just a 'surface' (as in scratching the) model... A proper one would involve everything down to bare nuclei, plus N stuff etc. But could be a way to start off DICE as a proper thing...

Ok, a real 'surface' model would just take the primary beam ionisations, but that wouldn't be any fun, would it?

Now a more interesting example would be could I construct a series of models similar to the electron one, but for each of the proton constituents (H, O, O2, N2), then find a way to coadd the resultant primary beams one by one?

That's it for today

Also sketched out an outline for the chapter relevant to this stuff

Next thing

Ok, the CTIPtype RIDE has lost its magnetic field. Next thing's to lose all the extraneous atmospheric species:

Current state of the modules:
randgen - No need to change
atom - Needs to be adjusted
cross - Needs adjusting
electron - Needs adjusting
strike - Needs adjusting
proton - Needs adjusting
proton1 - Needs adjusting
selectron - Needs adjusting
recoil - Needs adjusting
back - Needs adjusting
hit - Needs adjusting

Curent state of the input files:
NDens0 - Remains
NDens1 - Remains
NDens2 - Remains
NDens3 - Goes
NDens4 - Becomes NDens3
NDens5 - Goes
NDens6 - Goes
NDens7 - Goes
Temp - Remains

Note this is an intermediate step, which is why I don't just keep NDens1-3. I'm recreating RIDE from its own number densities before putting in the new ones.

Extraneous NDens' removed, N2 NDens renamed

Adjustments:
atom - adjusted arrays - done!
cross - adjusted echeck, adjusted ecross, adjusted cross - done!

Ok, for when I return:
electron
strike
proton
proton1
selectron
recoil
back
hit

Quick note

Have transfered Grodent's atmospheres, total H2 ionisation rates and subsequent H3+ densities into a spreadsheet. The first bit needs conversion so the five species can be used by RIDE properly. The second bit is the direct comparison between my ionisation rates and his. The final bit compares our chemistry models. Might be interesting...

I was a little worried that leakage of the 20keV maxwellian beyond RIDE's upper limit would cause problems with electrons not creating enough ionisation at the bottom of the atmosphere. However, the atmosphere cuts off before that point anyway...

More and more and more...

Computer problems to start the day off. Following the collapse of APL email, starlink email and UCL email, the APL server got fried.

Finished off Raman marking. Got given some mysterious scripts of Howarth that had evaded the last tranche of marking... odd. They were dealt with and returned to sender.

Also worked with Alex to create a second TIROS replacement, not linked to the BAS one. Could this mean I publish two new auroral oval models for the same atmospheric model in direct competition with each other? Not really, the BAS one is a substorm extension, the Alex one is a quiet time model, in effect we'll switch between them depending on what we're doing as the BAS one will be more computer intensive.

...and of course keep TIROS just incase something goes wrong...

But at least with Alex first stage is done, formatting the spectrum, chopping it up and deciding what will happen to it. The next stage is generating profiles, the third stage will then be doing all my little additions (literally back of the envelope, the envelope is next to the comp - I need a touch pad to doodle onto the Mac with) to conserve energy (yes that minor second law of thermodynamics thing). As Eddington said (ish), if your theory goes against Maxwell's equations, so much the worse for Maxwell, but if your theory contravenes the second law of thermodynamics, there's nothing to do but throw up your hands in defeat...

Must press the case for protons in both models...

Hmmm, looks like a million or so electrons will do for each of these levels. No adjustments required for RIDE to operate as it all ends at 30keV, well below RIDE's current nominal upper limit.

More

...of the same.

Saturn1000 finished the last of the 100keV GS runs, was analysed with no surprises or grade changes (though GS is now at the 90% complete mark along with BSR, whilst SD languishes at just above 70%). Saturn1000 is now running the 50eV GS1m run.

Now, Martian cross-sections, where was I?

Ionisation cross-sections now laboriously transferred.

Dissociation cross-sections now laboriously transferred. I think my fingers are now half their previous length...

eCheck and eLevel now adjusted (the arrays which say which species I have excitation cross-sections for (echeck) and what energy of excitation level this corresponds to (elevel)). The excitation cross-section array has also been suitably annexed. Cross now belongs to the Martians...

Module state of play:
randgen - ready
atom - ready
cross - ready
electron - needs conversion
strike - needs conversion
proton - needs conversion
proton1 - needs conversion
selectron - needs conversion
recoil - needs conversion
back - needs conversion
hit - needs conversion

...and the inputs are ok too. Also have a paper with energy spectrum to use if and when this gets ready to roll. Should I get the mag field, then the pitch angle spectrum is also available.

So, in the dying embers of the day, lets see what can be dealt with:
electron - Adjusted common blocks, declarations, code, compiled, done!
strike - adjusted common blocks, declarations, coded, compiled, done!
proton - adjusted common blocks, declarations, coded, compiled, done!
proton1 - adjusted common blocks, declarations, coded, compiled, done!
selectron - adjusted common blocks, declarations, coded, compile, done!
recoil - adjusted common blocks, declarations, coded, compiled, done!
back - adjusted common blocks, declarations, coded, compiled, done!
hit - adjusted common blocks, declarations, coded, compiled, done!

So, in theory a complete Martian model. Of course, a theoretically complete fortran model means only one thing - Segmentation faults lie in wait... we shall see.

And so we have... bastard thing. The debugger's no good too.

Right, trying Keter out, debugger works for once...

Model running

Model still running

Model still... WHY!!!! Did I wrong Mars in another life?

Suppose I'd better leave it there if it's going to run and run. Well, it won't go too long as I have imposed a twenty four hour limit on operations. We'll see if this thing really does work...

Have been told Anasuya's marking is now due!

Mars is finished. Really, finished... end of day.

More and more and more...

Ok, have extrapolated the Martian atmosphere. Now need to convert the various bits of terrestrial ride to another terrestrial planet.

Makefile states there are the following things to convert:
randgen - no conversion
atom - conversion
cross - conversion
electron - conversion
strike - conversion
proton - conversion
proton1 - conversion
selectron - conversion
recoil - conversion
back - conversion
hit - conversion

To which must be added:
NDens - all of them
MDip - convert eventually
MB - convert eventually
MDec - scrap
Temp - convert

Have so far converted all the NDenses, changed terrestrial species O, O2, N, N2, H, He, Ar and e- to O, O2, NO, N2, CO2, CO, Ar and e- - the Martian species.

Module conversion:
atom - converted (sounds like alchemy... just as scientific too)
Have since been mulling along with cross-sections. Found ionisation cross-sections for CO2 and CO, and have interpolated and extrapolated according to N2 shape factors to give full range cross-sections, however, not finished yet. Still need elastic scattering and dissociation cross-sections, not to mention dissociation and ionisation potentials, plus all the same info for NO... have created a new cross-section grid for mars including all the old Earth info for the cross-over species.

...that's it for today

More and more and more...

Saturn40 has finished the final 40eV GS run. This has been analysed, recoded and set off as an SD run. Analysis raises the 40eV grade to a first.

Some research done on Martian aurora. Altitude is about 129km, cf Martim altitude range of about 60-250km. Have got hold of a quick 1D Martian atmosphere to do a few runs on, but more cross-sections are required, as ever. The species involved are CO2, N2, O2, O, CO, NO and Ar. From the Earth, cross-sections are provided for N2, O2, O and Ar. This leaves CO2, CO and NO in need of some data, slightly unfortunate as the main emitting species is CO2 and other bands of interest include CO bands. Nevertheless, a quick browse about has netted a few cross-sections and as I know the names of the bands I need to work with, I can grab them - or at least have a better idea of where to look. A current and energy distribution have also been uncovered, suggesting a number flux can be determined, meaning I can then simulate a few emissions, see if they lie in the right area and are of the correct magnitude, then a more complex look should provide interesting things. Interesting things to look at include band emission ratios and the effect of pitch angle on all this, as field aligned electrons seem not to be dominant, apparently. We shall see.

The Martian atmosphere is a lot thinner than the Earth's, this means the number densities cover a very small altitude range, which in turn means a fast running program, hopefully. The low energy and flux of electrons involved in the Martian aurora should also help in that...

Atmosphere extrapolated. Tomorrow, I will create the program base.