Hill sphere

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File:Earth-moon-gravitational-potential.svg

In sectional/side view, a two-dimensional representation of the three-dimensional concept of the Hill sphere, here showing the Earth's "gravity well" (gravitational potential of Earth, blue line), the same for the Moon (red line) and their combined potential (black thick line). Point P is the force free spot, where gravitational forces of Earth and Moon cancel. The sizes of Earth and Moon are in the proportion, but distances and energies are not to scale.

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The Hill sphere is a common model for the calculation of a gravitational sphere of influence. It is the most commonly used model to calculate the spatial extent of gravitational influence of an astronomical body (m) in which it dominates over the gravitational influence of other bodies, particularly a primary (M).<ref name="Souami Cresson Biernacki Pierret p. ">Template:Cite journal</ref> It is sometimes confused with other models of gravitational influence, such as the Laplace sphere<ref name="Souami Cresson Biernacki Pierret p. "/> or being named the Roche sphere, the latter causing confusion with the Roche limit.<ref name="Williams 2015 w404">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref><ref name="Hill 2022 p. ">Template:Cite journal</ref> It was defined by the American astronomer George William Hill, based on the work of the French astronomer Édouard Roche.Template:Not verified in body

To be retained by a more gravitationally attracting astrophysical object—a planet by a more massive star, a moon by a more massive planet—the less massive body must have an orbit that lies within the gravitational potential represented by the more massive body's Hill sphere.Template:Not verified in body That moon would, in turn, have a Hill sphere of its own, and any object within that distance would tend to become a satellite of the moon, rather than of the planet itself.Template:Not verified in body

File:Lagrange points2.svg

A contour plot of the effective gravitational potential of a two-body system, here, the Sun and Earth, indicating the five Lagrange points.Template:Clarify Template:Citation needed

One simple view of the extent of the Solar System is that it is bounded by the Hill sphere of the Sun (engendered by the Sun's interaction with the galactic nucleus or other more massive stars).<ref name=Chebotarev1964>Template:Cite journal</ref>Template:Verify source A more complex example is the one at right, the Earth's Hill sphere, which extends between the Lagrange points Template:L1 and Template:L2,Template:Clarify which lie along the line of centers of the Earth and the more massive Sun.Template:Not verified in body The gravitational influence of the less massive body is least in that direction, and so it acts as the limiting factor for the size of the Hill sphere;Template:Clarify beyond that distance, a third object in orbit around the Earth would spend at least part of its orbit outside the Hill sphere, and would be progressively perturbed by the tidal forces of the more massive body, the Sun, eventually ending up orbiting the latter.Template:Not verified in body

For two massive bodies with gravitational potentials and any given energy of a third object of negligible mass interacting with them, one can define a zero-velocity surface in space which cannot be passed, the contour of the Jacobi integral.Template:Not verified in body When the object's energy is low, the zero-velocity surface completely surrounds the less massive body (of this restricted three-body system), which means the third object cannot escape; at higher energy, there will be one or more gaps or bottlenecks by which the third object may escape the less massive body and go into orbit around the more massive one.Template:Not verified in body If the energy is at the border between these two cases, then the third object cannot escape, but the zero-velocity surface confining it touches a larger zero-velocity surface around the less massive bodyTemplate:Verify source at one of the nearby Lagrange points, forming a cone-like point there.Template:Clarify Template:Not verified in body At the opposite side of the less massive body, the zero-velocity surface gets close to the other Lagrange point.Template:Not verified in body

DefinitionEdit

Template:Expand section The Hill radius or sphere (the latter defined by the former radiusTemplate:Citation needed) has been described as "the region around a planetary body where its own gravity (compared to that of the Sun or other nearby bodies) is the dominant force in attracting satellites," both natural and artificial.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>Template:Better source needed

As described by de Pater and Lissauer, all bodies within a system such as the Sun's Solar System "feel the gravitational force of one another", and while the motions of just two gravitationally interacting bodies—constituting a "two-body problem"—are "completely integrable ([meaning]...there exists one independent integral or constraint per degree of freedom)" and thus an exact, analytic solution, the interactions of three (or more) such bodies "cannot be deduced analytically", requiring instead solutions by numerical integration, when possible.<ref name=dePaterLissauerPlanetarySciences>Template:Cite book</ref>Template:Rp This is the case, unless the negligible mass of one of the three bodies allows approximation of the system as a two-body problem, known formally as a "restricted three-body problem".<ref name=dePaterLissauerPlanetarySciences/>Template:Rp

For such two- or restricted three-body problems as its simplest examples—e.g., one more massive primary astrophysical body, mass of <math>m_1</math>, and a less massive secondary body, mass of <math>m_2</math>—the concept of a Hill radius or sphere is of the approximate limit to the secondary mass's "gravitational dominance",<ref name=dePaterLissauerPlanetarySciences/> a limit defined by "the extent" of its Hill sphere, which is represented mathematically as follows:<ref name=dePaterLissauerPlanetarySciences/>Template:Rp<ref name=HiguchiIdaTAJapril2017>Template:Cite journal</ref>

<math>R_{\mathrm{H}} \approx a \sqrt[3]{\frac{m_2}{3(m_1+m_2)}}</math>,

where, in this representation, semi-major axis "<math>a</math>" can be understood as the "instantaneous heliocentric distance" between the two masses (elsewhere abbreviated rp).<ref name=dePaterLissauerPlanetarySciences/>Template:Rp<ref name=HiguchiIdaTAJapril2017/>

More generally, if the less massive body, <math>m_2</math>, orbits a more massive body, <math>m_1</math>(e.g., as a planet orbiting around the Sun), and has a semi-major axis <math>a</math>, and an eccentricity of <math>e</math>, then the Hill radius or sphere, <math>R_{\mathrm{H}}</math> of the less massive body, calculated at the pericenter, is approximately:<ref name="HamiltonBurns92">Template:Cite journal See also Template:Cite journal cited therein.</ref>Template:Primary source inline Template:Better source needed

<math>R_{\mathrm{H}} \approx a (1-e) \sqrt[3]{\frac{m_2}{3(m_1+m_2)}}.</math>

When eccentricity is negligible (the most favourable case for orbital stability), this expression reduces to the one presented above.Template:Citation needed

Example and derivationEdit

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File:Comparison of Hill sphere and Roche limit.svg

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In the Earth-Sun example, the Earth (Template:Val) orbits the Sun (Template:Val) at a distance of 149.6 million km, or one astronomical unit (AU). The Hill sphere for Earth thus extends out to about 1.5 million km (0.01 AU). The Moon's orbit, at a distance of 0.384 million km from Earth, is comfortably within the gravitational sphere of influence of Earth and it is therefore not at risk of being pulled into an independent orbit around the Sun.

The earlier eccentricity-ignoring formula can be re-stated as follows:

<math>\frac{R^3_{\mathrm{H}}}{a^3} \approx 1/3 \frac{m2}{M}</math>, or <math>3\frac{R^3_{\mathrm{H}}}{a^3} \approx \frac{m2}{M}</math>,

where M is the sum of the interacting masses.

DerivationEdit

{{ safesubst:#invoke:Unsubst||date=__DATE__ |$B= {{ safesubst:#invoke:Unsubst||date=__DATE__ |$B= Template:Ambox }} }} The expression for the Hill radius can be found by equating gravitational and centrifugal forces acting on a test particle (of mass much smaller than <math>m</math>) orbiting the secondary body. Assume that the distance between masses <math>M</math> and <math>m</math> is <math>r</math>, and that the test particle is orbiting at a distance <math>r_{\mathrm{H}}</math> from the secondary. When the test particle is on the line connecting the primary and the secondary body, the force balance requires that

<math>\frac{Gm}{r^2_{\mathrm{H}}}-\frac{GM}{(r-r_{\mathrm{H}})^2}+\Omega^2(r-r_{\mathrm{H}})=0,</math>

where <math>G</math> is the gravitational constant and <math>\Omega=\sqrt{\frac{GM}{r^3}}</math> is the (Keplerian) angular velocity of the secondary about the primary (assuming that <math>m\ll M</math>). The above equation can also be written as

<math>\frac{m}{r^2_{\mathrm{H}}}-\frac{M}{r^2}\left(1-\frac{r_{\mathrm{H}}}{r}\right)^{-2}+\frac{M}{r^2}\left(1-\frac{r_{\mathrm{H}}}{r}\right)=0,</math>

which, through a binomial expansion to leading order in <math>r_{\mathrm{H}}/r</math>, can be written as

<math>\frac{m}{r^2_{\mathrm{H}}}-\frac{M}{r^2}\left(1+2\frac{r_{\mathrm{H}}}{r}\right)+\frac{M}{r^2}\left(1-\frac{r_{\mathrm{H}}}{r}\right) = \frac{m}{r^2_{\mathrm{H}}}-\frac{M}{r^2}\left(3\frac{r_{\mathrm{H}}}{r}\right)\approx 0.</math>

Hence, the relation stated above

<math>\frac{r_{\mathrm{H}}}{r}\approx \sqrt[3]{\frac{m}{3 M}}.</math>

If the orbit of the secondary about the primary is elliptical, the Hill radius is maximum at the apocenter, where <math>r</math> is largest, and minimum at the pericenter of the orbit. Therefore, for purposes of stability of test particles (for example, of small satellites), the Hill radius at the pericenter distance needs to be considered.

To leading order in <math>r_{\mathrm{H}}/r</math>, the Hill radius above also represents the distance of the Lagrangian point L₁ from the secondary.

Regions of stabilityEdit

Template:Cleanup reorganize The Hill sphere is only an approximation, and other forces (such as radiation pressure or the Yarkovsky effect) can eventually perturb an object out of the sphere.Template:Citation needed As stated, the satellite (third mass) should be small enough that its gravity contributes negligibly.<ref name=dePaterLissauerPlanetarySciences/>Template:Rp

The region of stability for retrograde orbits at a large distance from the primary is larger than the region for prograde orbits at a large distance from the primary. This was thought to explain the preponderance of retrograde moons around Jupiter; however, Saturn has a more even mix of retrograde/prograde moons so the reasons are more complicated.<ref>Template:Cite journal</ref> In a two-planet system, the mutual Hill radius of the two planets must exceed <math>2\sqrt{3}</math> to be stable. Multi-planet systems of three or more with semi-major-axis differences of less than ten mutual Hill radii are always unstable. This is due to the loss of angular momentum due to perturbations by a third planet.<ref>Chambers, J. E., Wetherill, G. W., & Boss, A. P. (1996). The stability of multi-planet systems. Icarus, 119(2), 261-268.</ref>

Further examplesEdit

Template:More citations needed section It is possible for a Hill sphere to be so small that it is impossible to maintain an orbit around a body. For example, an astronaut could not have orbited the 104 ton Space Shuttle at an orbit 300 km above the Earth, because a 104-ton object at that altitude has a Hill sphere of only 120 cm in radius, much smaller than a Space Shuttle. A sphere of this size and mass would be denser than lead, and indeed, in low Earth orbit, a spherical body must be more dense than lead in order to fit inside its own Hill sphere, or else it will be incapable of supporting an orbit. Satellites further out in geostationary orbit, however, would only need to be more than 6% of the density of water to fit inside their own Hill sphere.Template:Citation needed

Within the Solar System, the planet with the largest Hill radius is Neptune, with 116 million km, or 0.775 au; its great distance from the Sun amply compensates for its small mass relative to Jupiter (whose own Hill radius measures 53 million km). An asteroid from the asteroid belt will have a Hill sphere that can reach 220,000 km (for 1 Ceres), diminishing rapidly with decreasing mass. The Hill sphere of 66391 Moshup, a Mercury-crossing asteroid that has a moon (named Squannit), measures 22 km in radius.<ref name="Moshup">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

A typical extrasolar "hot Jupiter", HD 209458 b,<ref>Template:Cite encyclopedia</ref> has a Hill sphere radius of 593,000 km, about eight times its physical radius of approx 71,000 km. Even the smallest close-in extrasolar planet, CoRoT-7b,<ref>Template:Cite encyclopedia</ref> still has a Hill sphere radius (61,000 km), six times its physical radius (approx 10,000 km). Therefore, these planets could have small moons close in, although not within their respective Roche limits.Template:Citation needed

Hill spheres for the solar systemEdit

The following table and logarithmic plot show the radius of the Hill spheres of some bodies of the Solar System calculated with the first formula stated above (including orbital eccentricity), using values obtained from the JPL DE405 ephemeris and from the NASA Solar System Exploration website.<ref name="mnras_style">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Radius of the Hill spheres of some bodies of the Solar System
Body	Million km	au	Body radii	Arcminutes<ref group="note">At average distance, as seen from the Sun. The angular size as seen from Earth varies depending on Earth's proximity to the object.</ref>	Farthest moon (au)	Ratio of farthest moon to Hill sphere radius
Mercury	0.1753	0.0012	71.9	10.7	Template:NA	Template:NA
Venus	1.0042	0.0067	165.9	31.8	Template:NA	Template:NA
Earth	1.4714	0.0098	230.7	33.7	0.00257	0.262
Mars	0.9827	0.0066	289.3	14.9	0.00016	0.242
Jupiter	50.5736	0.3381	707.4	223.2	0.1662	0.491
Saturn	61.6340	0.4120	1022.7	147.8	0.1785	0.433
Uranus	66.7831	0.4464	2613.1	80.0	0.1366	0.306
Neptune	115.0307	0.7689	4644.6	87.9	0.3360	0.437
Ceres	0.2048	0.0014	433.0	1.7	Template:NA	Template:NA
Pluto	5.9921	0.0401	5048.1	3.5	0.00043	0.0107
Eris	8.1176	0.0543	6979.9	2.7	0.00025	0.0046

File:Hill sphere of the planets.png

Logarithmic plot of the Hill radii (in km) for the bodies of the solar system

Explanatory notesEdit

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ReferencesEdit

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External linksEdit

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