NASA AP8/AE8. Models of proton and electron fluxes in the Earth's radiation belts.
This software is the program that computes omnidirectional, integral, or differential (in energy) fluxes of electrons and protons trapped in Earth's radiation belts for specified energy, L-value, and B/B0 range. The fluxes are obtained by an interpolation procedure from the experimental data. The program allows the user to specify input parameters and options from file and generates flux tables that stored to file.
Program based on radbelt package that you can to download from the developer site.
Fortran source of radbelt can be downloaded from nssdcftp.gsfc.nasa.gov
Unfortunately radbelt was written too long ago and it's too difficult to compile it. I tried to use Salford Software FTN 95, Intel Fortran, but they tell me that there is a lot of syntax errors in program. WATCOM FORTRAN/77 Ver.1.4 on WindowsXP SP2 could compile this program after fixing two minor bugs.
Original program radbelt, written by Dieter Bilitza is interactive, i.e. it asks a lot of questions - where we want to calculate flux, which model it have to use, to write output to file or to screen. After that actions program works. But the calculation of flux in one-two point is not enough in most cases. And we need to find model flux in wide ranges of longitudes and latitudes on some altitude. For this case NASA program is not useful. Fortunately radbelt is the interface to trmfun library. After the thoughtfully investigation of program I rewrite it. Now program can take energy ranges, geomagnetic coordinates and model type from file and writes calculation to file.
In the beginning of working the program will ask you names of input and output files.
It should be noticed that in your working directory had not to be file with name of output file. Delete old files yourself.
Input file should contain lines of following format:
L B/B0 MODEL FLUXTYPE E1 E2
Example:
2.15 2.5 2 1 0.5 0.7
Where:
L - McIlwein parameter,
B/B0 - fraction of magnetic field strength in the position of observer and in the position of field line top.
MODEL - one of following integer numbers, flux model:
1 AP8MAX, protons, solar maximum
2 AP8MIN, protons, solar minimum
3 AE4MAX, electrons, solar maximum
4 AE4MIN, electrons, solar minimum
5 AEI7HI, electrons, high estimate
6 AEI7LO, electrons, low estimate
7 AE8MAX, electrons, solar maximum
8 AE8MIN, electrons, solar minimum
FLUXTYPE - one of following integer numbers, selection of flux type: 1 - integral 2 - differential
E1 - for integral flux - threshold of energy (MeV), to calculate Flux(>E1),
for differential - lowest threshold of energy (MeV) to calculate Flux(E1<E<E2)
E2 - for integral flux program doesn't take this number into account
for differential - highest threshold of energy (MeV) to calculate Flux(E1<E<E2)
As the result of program work file of following format will be generated:
L B/B0 MODEL FLUXTYPE E1 E2 FLUX1 2.1500001 2.5000000 2.0000000 1.0000000 0.5000000 0.7000000 1.2473444E+006
Where L, B/B0, MODEL, FLUXTYPE, E1, E2 are the same as in input file, but integer numbers obtain decimal part.
The last column FLUX1 means flux calculated using model of selected name.
Integral flux units are particles/(cm*cm*sec), differential flux units are particles/(cm*cm*sec*MeV)
