madsmh
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How does one correct for tidal forces when (classically) simulating the orbits of solar system bodies?
The discussion revolves around the correction for tidal forces in classical simulations of solar system bodies' orbits, particularly focusing on the larger moons of Jupiter. Participants explore the impact of tidal effects and planetary oblateness on simulation accuracy, raising questions about integration methods and the influence of mutual interactions among celestial bodies.
Participants do not reach a consensus on the causes of the errors in the simulations, with multiple competing views regarding the roles of tidal forces, oblateness, and integration methods. The discussion remains unresolved as participants continue to explore these issues.
Limitations include the dependence on assumptions about the shapes of celestial bodies, the complexity of tidal interactions, and the unresolved nature of the mathematical steps involved in correcting for oblateness and tidal effects.
Calculating and predicting the change in lunar rotation and orbit seems to be fairly do-able or so they claim.mfb said:Tidal forces don't affect the motion of the center of mass unless the object is notably different from a sphere. If that is relevant, just calculate how large the effect is and take it into account.
I would expect an issue with the integration scheme. How does the difference change if you change the step size? How many moons with mutual interactions do you consider? Do you consider the other planets?madsmh said:Thanks, can you point me to some resources on how to do that?
I am making a solar system simulator, and the errors I get when simulating the larger moons of Jupiter are about the diameter of their orbits when simulating three years. I have made some animations and can see that they fall behind their reference positions quite early in the simulations. And my current hypothesis is that it's due to tidal effects.
Huh?madsmh said:6 Saturn: 179597 km