AstrodynamicalCalculations.jl
Common calculations within orbital mechanics and astrodynamics.
AstrodynamicalCalculations — ModuleCommon calculations within orbital mechanics and astrodynamics.
Extended Help
Imports
AstrodynamicalCalculations.CR3BPCalculationsAstrodynamicalCalculations.R2BPCalculationsBaseCoreDocStringExtensionsReexport
Exports
CR3BPCalculationsR2BPCalculationsapoapsis_radiusargument_of_periapsisc3cartesian_to_kepleriancartesian_to_perifocalconicconvergeconverge!convergent_directiondistance_scalingdistance_to_primarydistance_to_secondarydivergediverge!divergent_directioneccentricityeccentricity_vectorhohmanninclinationjacobi_constantkeplerkeplerian_to_cartesiankeplerian_to_perifocallagrange_pointlambertmean_motionnondimensionalnondimensional_radiiorbital_periodorbital_radiusorbital_speedperiapsis_radiusperifocal_to_cartesianperturbperturb!perturbationpotential_energyprimary_synodic_positionredimensionedreduced_massrichardson_halorichardson_icright_ascension_ascending_nodesecondary_synodic_positionsemi_parametersemimajor_axisspecific_angular_momentumspecific_angular_momentum_vectorspecific_energyspecific_potential_energysphere_of_activitysphere_of_influencetime_scalingtime_since_periapsistrue_anomalyv_infinityvelocity_scalingzero_velocity_curves
Installation
pkg> add AstrodynamicalCalculationsGetting Started
One common task within first-year orbital mechanics courses is converting to, and from, Keplerian parameters (orbital elements). Kepler's prediction algorithm is another staple! These simple calculations are provided by the R2BPCalculations submodule within AstrodynamicalCalculations.
The size of all of the vectors in these calculations are known at compile time. You can drastically improve performance by using StaticArrays types, i.e. SVector.
julia> using AstrodynamicalCalculations
julia> r = [0.0, 11681.0, 0.0]; # km
julia> v = [5.134, 4.226, 2.787]; # km/s
julia> μ = 398600.4354360959; # km³ s⁻²
julia> e, a, i, Ω, ω, ν = cartesian_to_keplerian(r, v, μ)
(0.723452708202361, 24509.265399338536, 2.6442542356744734, 1.5707963267948966, 4.712449617676915, 1.5707356895026707)
julia> T = orbital_period(a, μ)
38186.19850882009
julia> rₙ, vₙ = kepler(r, v, μ, 2.5T)
([36872.96963754877, -2574.241491333036, 20016.549742861007], [-0.3141726028666592, -1.6044679459972122, -0.17054909314167882])