High Precision Orbit Propagator

Precise modeling of satellite's perturbed motion (special perturbations approach)

The motion of a near-Earth satellite is affected by various forces. One of these forces is the Earth's central gravitation and the others are known as perturbations. These perturbations are classified into gravitational and non-gravitational forces. In this case, the equation of motion can be written as:

r ̈=-(GM/r^3)*r+γ_p

γ_p is the vector of additional accelerations induced by the disturbing forces.

γ_p=r ̈_E+r ̈_S+r ̈_M+r ̈_P+r ̈_e+r ̈_o+r ̈_D+r ̈_SP+r ̈_A+r ̈_emp

r ̈_E = Accelerations due to the non-spherically and inhomogeneous mass distribution within Earth (central body)

r ̈_S, r ̈_M, r ̈_P = Accelerations due to other celestial bodies (Sun, Moon, and planets)

r ̈_e, r ̈_o = Accelerations due to Earth and oceanic tides

r ̈_D = Accelerations due to atmospheric drag

r ̈_SP, r ̈_A = Accelerations due to direct and Earth-reflected solar radiation pressure

r ̈_emp = Accelerations due to unmodeled forces

Here I have used the following integrator and force model to simulate the satellite's perturbed motion:

Integrator: Runge-Kutta-Fehlberg 7(8)

Force Model:

- gravity field of the Earth (GGM03C model)

- gravity of the solar system planets (positions of the planets are computed by JPLDE440)

- drag effect using NRLMSISE-00, Jacchia-Bowman 2006 & 2008, MSIS-86, Jacchia 70, or modified Harris-Priester atmospheric density model (in Accel.m you can uncomment your favorite model)

- solar radiation pressure using conical, geometrical, or cylindrical shadow model

- solid Earth tides (IERS Conventions 2010)

- ocean tides

- general relativity

- ECEF2ECI and ECI2ECEF transformations using IAU 2006 Resolutions

The Simulation starts by running the test_HPOP.m. In the InitialState.txt set initial values for your favorite satellite; lines 2-7 are the state vector of satellite/spacecraft in the International Terrestrial Reference Frame (ITRF). Lines 8 to 12 are the satellite parameters related to the forces from atmospheric drag and solar radiation pressure. Lines 8-10 are in units m^2 and kg. Line 11: Cr is the radiation pressure coefficient (Cr = 1 + reflectivity of satellite). Line 12: Cd is the atmospheric drag coefficient of the satellite. In the test_HPOP.m you can consider different perturbations by setting them 1 as follows:

AuxParam.n = 70; % maximum degree of central body's gravitation field

AuxParam.m = 70; % minimum order of central body's gravitation field

AuxParam.sun = 1; % perturbation of the Sun

AuxParam.moon = 1; % perturbation of Moon

AuxParam.planets = 1; % perturbations of planets

AuxParam.sRad = 1; % solar radiation pressure

AuxParam.drag = 1; % atmospheric drag

AuxParam.SolidEarthTides = 1; % solid Earth tides

AuxParam.OceanTides = 1; % ocean tides

AuxParam.Relativity = 1; % general relativity

References:

Montenbruck O., Gill E.; Satellite Orbits: Models, Methods and Applications; Springer Verlag, Heidelberg; Corrected 3rd Printing (2005).

Montenbruck O., Pfleger T.; Astronomy on the Personal Computer; Springer Verlag, Heidelberg; 4th edition (2000).

Seeber G.; Satellite Geodesy; Walter de Gruyter, Berlin, New York; 2nd completely revised and extended edition (2003).

Vallado D. A; Fundamentals of Astrodynamics and Applications; McGraw-Hill, New York; 4th edition (2013).

NIMA. 2000. Department of Defense World Geodetic System 1984. NIMA-TR 8350.2, 3rd ed, Amendment 1. Washington, DC: Headquarters, National Imagery, and Mapping Agency.

http://celestrak.org/SpaceData/EOP-All.txt

http://celestrak.org/SpaceData/SW-All.txt

https://sol.spacenvironment.net/JB2008/indices/SOLFSMY.TXT

https://sol.spacenvironment.net/JB2008/indices/SOLRESAP.TXT

https://sol.spacenvironment.net/JB2008/indices/DTCFILE.TXT

https://ssd.jpl.nasa.gov/planets/eph_export.html