Deriving the Effect of Solar Radiation Pressure on Orbits
A simple method for adding solar radiation perturbations to a two-body problem model
Orbits of smaller bodies, such as satellites, asteroids, comets, etc., can be quite complex. Typical mission planning includes solving the two-body problem to obtain a basic orbit. From there, complexities such as perturbing forces can be added to increase the accuracy of the model. With respect to orbital mechanics, a perturbation (or perturbing force) is a force acting on a mass other than the gravitational pull of a single other massive body. These forces can be difficult to model, but with the right mindset and understanding, they can be simplified substantially.
Perturbations
Perturbing forces can be broken down into two categories: gravitational forces or non-gravitational forces. In the gravitational forces category, we have forces such as tidal forces, gravitational pull of other massive bodies, and the effects of an oblate attracting body. The non-gravitational perturbing forces are atmospheric drag, radiation pressure, and magnetic forces. All of these forces should be considered when building a high-fidelity (high accuracy) orbit model. The effects of these forces can be crucial for mission success.
