Science Fair Project Encyclopedia
A Hill sphere approximates the gravitational sphere of influence of one astronomical body in the face of perturbations from another heavier body around which it orbits. It was defined by the American astronomer George William Hill. It is also called the Roche sphere because the French astronomer Édouard Roche independently described it.
- gravity due to the central body
- gravity due to the second body
- the centrifugal force in a frame of reference rotating about the central body with the same angular frequency as the second body (Jupiter)
The Hill sphere is the largest sphere within which the sum of the three fields is directed towards the second body. A small third body can orbit the second within the Hill sphere, with this resultant force as centripetal force.
The Hill sphere extends between the Lagrangian points L1 and L2, which lie along the line of centers of the two bodies. The region of influence of the second body is shortest in that direction, and so it acts as the limiting factor for the size of the Hill sphere. Beyond that distance, a third object in orbit around the second (Jupiter) would spend at least part of its orbit outside the Hill sphere, and would be progressively perturbed by the tidal forces of the central body (the Sun) and would end up orbiting the latter.
Formula and examples
If the mass of the smaller body is m, and it orbits a heavier body of mass M at a distance a, the radius r of the Hill sphere of the smaller body is
For example, the Earth (5.97×1024 kg) orbits the Sun (1.99×1030 kg) at a distance of 149.6 Gm. The Hill sphere for Earth thus extends out to about 1.5 Gm (0.01 AU). The Moon's orbit, at a distance of 0.370 Gm from Earth, is comfortably within the gravitational sphere of influence of Earth and is therefore not at risk of being pulled into an independent orbit around the Sun. In terms of orbital period: the Moon has to be within the sphere where the orbital period is not more than 7 months.
An astronaut could not orbit the Space Shuttle (mass = 104 tonnes), if the orbit is 300 km above the Earth, since the Hill sphere is only 120 cm in radius, much smaller than the shuttle itself. In fact, in any low Earth orbit, a spherical body must be 800 times denser than lead in order to fit inside its own Hill sphere, or else it will be incapable of supporting an orbit. A spherical geostationary satellite would need to be more than 5 times denser than lead to support satellites of its own; such a satellite would be 2.5 times denser than iridium, the densest naturally-occurring material on Earth. Only at twice the geostationary distance could a lead sphere possibly support its own satellite; the moon itself must be at least 3 times the geostationary distance, or 2/7 its present distance, to make lunar orbits possible.
The Hill sphere is but an approximation, and other forces (such as radiation pressure) can make an object deviate from within the sphere. The third object must also be of small enough mass that it introduces no additional complications through its own gravity. Orbits at or just within the Hill sphere are not stable in the long term; from numerical methods it appears that stable satellite orbits are inside 1/2 to 1/3 of the Hill radius (with retrograde orbits being more stable than prograde orbits).
Within the solar system, the planet with the largest Hill sphere is Neptune, with 116 Gm, or 0.775 AU; its great distance from the Sun amply compensates for its small mass relative to Jupiter (whose own Hill sphere measures 53 Gm). An asteroid from the main belt will have a Hill sphere that can reach 220 Mm (for 1 Ceres), diminishing rapidly with its mass. In the case of (66391) 1999 KW4, a Mercury-crosser asteroid which has a moon (S/2001 (66391) 1), the Hill sphere varies between 120 and 22 km in radius depending on whether the asteroid is at its aphelion or perihelion!
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