Work!

Makenzie has produced a corrected profile to be modelled. That with Alex's stuff should keep me going (plus validation graphs).

But first - marking. Now done (Howarth that is... have asked Raman and should get his stuff tomorrow/monday)

Supercomputer queues are to be altered again, making it possible to rerun the six 'dead' runs.

Have spoken with Alex about the proton oval

Also have interpolated out the CTIP atmosphere for the runs. I have the energies from the DMSP thing, bit worried about not having H, He at least (also N and Ar), which could reduce the overall ionisation rate (not so much Ar, but at the top, definately H and He). We shall see... shouldn't be too bad as O remains about ten times the next thing, and has a larger cross-section...

...even so...

Oh yes, and attended Steve's H3+ talk. As well as a later one involving Makenzie's profile...

So, now marking's over what's left to do?

Alex stuff - 19 runs of a million electrons into a modified version of RIDE Earth according to DMSP energies
Makenzie stuff - fit profile (there, sounds easy)
Grodent stuff - validation
Thesis stuff - write up whichever of the above gets done first...

Marking - whenever

we'll see...

Have checked the Ovation model Alex/George are using to define the auroral oval - it includes ions!

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...