Orbital Determination via the Method of Gauss
Original version 07/22/2016, SSP NMT 2016
Current version: 2.0.0 (09/19/2016)
Run the code from the command line like so:
python main.py <input-file-path>
You will be prompted to pick a root by the program after a second. Pick a distance (in AU) that is reasonable for the class of asteroid you are observing. Wait for the code to run through the iteration and print out your data at the end if you feel the need.
##Input file format
The format of the input file is very specific in order but is tolerant in some regards, like the number of decimal places in the sun-earth vector components, time, or coordinates.
An example input file might look like:
10150 (1994 PN) 2016-06-22 08:03:10.429 17:26:58.87 30:46:11.30 -0.0195340791840548 0.9323384266123208 0.4041408400938959 2016-06-30 07:19:24.379 17:08:12.58 27:19:02.51 -0.1537983334829756 0.9221125109705270 0.3997035045290656 2016-07-07 05:21:27.350 16:51:52.97 23:04:41.48 -0.2682470588825682 0.8998279354659114 0.3900449087482382 2016-07-13 03:42:48.670 16:38:37.64 18:31:04.40 -0.3635214279037087 0.8710218039698151 0.3775632429881836
With the format of each line being:
Date Time RA(HMS) Dec(DMS) Sun-Earth Vector (AU) YYYY-MM-DD HH:MM:SS.s HH:MM:SS.ss DD:MM:SS.ss X Y Z
##Further Reading For more information about the Method of Gauss and the calculations contained within, please consult this document.