madsmh
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How does one correct for tidal forces when (classically) simulating the orbits of solar system bodies?
This discussion focuses on correcting tidal forces and planetary oblateness in solar system simulations, particularly for the larger moons of Jupiter. The user reports significant errors in their simulation, with deviations reaching the diameter of the orbits over three years. They utilize the Velocity Verlet integration scheme and have identified that the oblateness of celestial bodies, especially Jupiter, contributes to these inaccuracies. The user successfully implemented corrections for oblateness, improving the accuracy of Europa's position significantly.
PREREQUISITESAstronomers, astrophysicists, and developers of simulation software who are focused on improving the accuracy of celestial mechanics simulations, particularly those involving tidal forces and planetary oblateness.
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