This is a list of additions, enhancements, corrections, etc., that I am currently working on or thinking about, which hopefully will be included in the next release of the GLOW model, anticipated for 2019. Anybody that wants to volunteer to work on one of these, feel free. LBH thresholding Correct solar irradiance for Sun-Earth distance Green line recombination emission O2 A-bands emission Ion chemistry re-examination Option for parameterized auroral proton ionization rate (done!) Update magnetic field used in FIELDM and GEOMAG Re-install conjugate photoelectrons as an option Update IRI WACCM-X interface for driver program Fix electron heating rate Add He, H, He+, and H+ Add cusp and drizzle fluxes from TGCMs Re-write EXSECT for table-based electron impact cross-sections Discussion: LBH thresholding: This means putting in different cross sections for each v' upper state, each of which has a different threshold. The approach will be to use a total cross section for N2(a) in the energetic electron redistribution array, but individual cross sections for each v' in the excitation calculation. That will be done in the new subroutine BANDS, which also could handle collisional/cascade re-distribution. Correct solar irradiance for Sun-Earth distance: Nobody ever thought we knew solar EUV to anything close to 7% accuracy, so I never worried about this before. Now, with improved measurements, it seems worth bothering to put it in. Also should correct solar zenith angle for Earth oblateness. As is, it is accurate to within <0.2 degrees. Also note that the value of F10.7 input to MSIS should actually be the measured value at Earth, not the 1 AU value, which means that it should be corrected for Sun-Earth distance. Green line recombination emission: This has been on the list for decades. Just haven't gotten around to it, because it isn't important above ~100 km, for projects I've been working on. But it needs to be done. Could be done by solving for all the O2 Hertzberg upper states, or as a specific recombination rate, skipping the details, which brings us to... O2 A-bands emission: Also long overdue. All the pieces for the thermospheric components are there, but need to deal with recombination, and O3 if we go into the mesosphere. Ion chemistry re-examination: I would like to bring GLOW into general agreement with Richards [2011] who did a great job with this. The only reason it hasn't happened yet is that ion chemistry is not the prime mission here, but it can be important, especially for aurora, and daytime E-region. Option for parameterized auroral proton ionization rate: This is new in v0.982. Calculates electron density profiles and conductivities, but does not produce secondaries and emission features. Note, however, that secondary electron ionization is included in the parameterization. Next step for protons is to generate secondary electrons and include in ETRANS. Update magnetic field used in FIELDM and GEOMAG: This is overdue for an overhaul, but lower priority because FIELDM's only job is to calculate the dip angle, and electron transport is weakly dependent on dip angle. GEOMAG now only handles coordinate transforms for the NOEM nitric oxide model, which is based on SNOE data that were analyzed with a simple offset-tilted-dipole model to begin with. Nevertheless, I'd like to consolidate these using IGRF and Apex coordinates, including secular variation, using the standard TGCM method. This would also make the conjugate electron calculation (currently deprecated) more accurate. Re-install conjugate photoelectrons as an option: This is easily recovered from v. 0.97, but I took it out because of the above, because it is a large performance hit for global calculations, and because it wasn't really in use. Update IRI: Many might wonder why GLOW still uses IRI-90 as its default empirical a-priori ionosphere. The reasons are that GLOW generally only uses a-priori electron density above 200 km, and the F-region in IRI hasn't changed much. Also, the new versions of IRI come with their own input files, imbedded MSIS calls, and many options that aren't needed by GLOW. I need to strip out all the paraphernalia, and create a simple subroutine interface, similar to what is now used for IRI-90. It's a lot of messing around with OPC and I'm hoping somebody else will do it. WACCM-X interface for driver program: This will be similar to the READTGCM module. Any help appreciated! Fix electron heating rate: Electron heating rates are calculated, but approximate, because there isn't enough energy bin resolution below ~1 eV and because of the way the the bottom bin is treated. Light atoms and ions: He and H are available from empirical and/or numerical models and can be added easily, ionization rates and charge exchange chemistry could then be incorporated. I anticipate that they would be treated as minor species, i.e., neglecting contributions to absorption and photoelectron generation, as is currently done with N and NO. Add cusp and drizzle fluxes from TGCMs: These can be specified on TGCM secondary histories, and are included in readtgcm; just need a simple interface to generate the appropriate energetic electrons into ETRANS. Re-write EXSECT for table-based cross-section input: This isn't really a low priority, in fact it might be the highest priority, especially because some people have complained about how inflexible the heritage cross section method is. At the same time, I need to re-evaluate cross sections, and break out the lumped states, espcially the N2 singlets because of the importance of LBH, but also the N2 triplets and O2 Hertzbergs. The reason this is at the bottom of the list is that it is a lot of work, in part because the secondary electron production is bound up in the analytic ionization cross-section method, and also because EXSECT has some of the oldest and messiest of all the GLOW code.