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If k 2 is greater than one, F 2 − F 1 is a negative number; thus, the added inverse-cube force is attractive, as observed in the green planet of Figures 1–4 and 9. By contrast, if k 2 is less than one, F 2 − F 1 is a positive number; the added inverse-cube force is repulsive , as observed in the green planet of Figures 5 and 10, and in ...
Nodal precession is the precession of the orbital plane of a satellite around the rotational axis of an astronomical body such as Earth.This precession is due to the non-spherical nature of a rotating body, which creates a non-uniform gravitational field.
The common noun ‘moon’ (not capitalized) is used to mean any natural satellite of the other planets. Tidal force is the combination of out-of-balance forces and accelerations of (mostly) solid bodies that raises tides in bodies of liquid (oceans), atmospheres, and strains planets' and satellites' crusts.
The planet-fixed values of v and θ are converted to space-fixed (inertial) values with the following conversions: [7] = + + (), where ω is the planet's rotational rate in radians per second, φ is the launch site latitude, and A z is the launch azimuth angle.
Basically, there are also torques from other planets that cause planetary precession which contributes to about 2% of the total precession. Because periodic variations in the torques from the sun and the moon, the wobbling (nutation) comes into place. You can think of precession as the average and nutation as the instantaneous.
All eight planets in the Solar System orbit the Sun in the direction of the Sun's rotation, which is counterclockwise when viewed from above the Sun's north pole. Six of the planets also rotate about their axis in this same direction. The exceptions – the planets with retrograde rotation – are Venus and Uranus.
In astronomy, the rotation period or spin period [1] of a celestial object (e.g., star, planet, moon, asteroid) has two definitions. The first one corresponds to the sidereal rotation period (or sidereal day), i.e., the time that the object takes to complete a full rotation around its axis relative to the background stars (inertial space).
In Mercury's case, the planet completes three rotations for every two revolutions around the Sun, a 3:2 spin–orbit resonance. In the special case where an orbit is nearly circular and the body's rotation axis is not significantly tilted, such as the Moon, tidal locking results in the same hemisphere of the revolving object constantly facing ...