Roche limit

This article is about the orbit within which particles might form rings or objects on a stable orbit might disintegrate into rings. For the limits at which an orbiting object will be captured, see Roche lobe. For the gravitational sphere of influence of one astronomical body in the face of perturbations from another heavier body around which it orbits, see Roche sphere.

In celestial mechanics, the Roche limit, also called Roche radius, is the distance from a celestial body within which a second celestial body, held together only by its own force of gravity, will disintegrate because the first body's tidal forces exceed the second body's self-gravitation.^[1] Inside the Roche limit, orbiting material disperses and forms rings, whereas outside the limit, material tends to coalesce. The Roche radius depends on the radius of the first body and on the ratio of the bodies' densities.

A celestial body (yellow) is orbited by a mass of fluid (blue) held together by gravity, here viewed from above the orbital plane. Far from the Roche limit (white line), the mass is practically spherical.

Closer to the Roche limit, the body is deformed by tidal forces.

Within the Roche limit, the mass's own gravity can no longer withstand the tidal forces, and the body disintegrates.

Particles closer to the primary move more quickly than particles farther away, as represented by the red arrows.

The varying orbital speed of the material eventually causes it to form a ring.

The term is named after Édouard Roche (French: [ʁɔʃ], English: /rɒʃ/ ROSH), the French astronomer who first calculated this theoretical limit in 1848.^[2]

Explanation

Comet Shoemaker-Levy 9 was disintegrated by the tidal forces of Jupiter into a string of smaller bodies in 1992, before colliding with the planet in 1994.

The Roche limit typically applies to a satellite's disintegrating due to tidal forces induced by its primary, the body around which it orbits. Parts of the satellite that are closer to the primary are attracted more strongly by gravity from the primary than parts that are farther away; this disparity effectively pulls the near and far parts of the satellite apart from each other, and if the disparity (combined with any centrifugal effects due to the object's spin) is larger than the force of gravity holding the satellite together, it can pull the satellite apart. Some real satellites, both natural and artificial, can orbit within their Roche limits because they are held together by forces other than gravitation. Objects resting on the surface of such a satellite would be lifted away by tidal forces. A weaker satellite, such as a comet, could be broken up when it passes within its Roche limit.

Since, within the Roche limit, tidal forces overwhelm the gravitational forces that might otherwise hold the satellite together, no satellite can gravitationally coalesce out of smaller particles within that limit. Indeed, almost all known planetary rings are located within their Roche limit. (Notable exceptions are Saturn's E-Ring and Phoebe ring. These two rings could possibly be remnants from the planet's proto-planetary accretion disc that failed to coalesce into moonlets, or conversely have formed when a moon passed within its Roche limit and broke apart.)

The gravitational effects occurring below the Roche limit is not the only factor that causes comets to break apart. Splitting by thermal stress, internal gas pressure and rotational splitting are other ways for a comet to split under stress.

Determination

The limiting distance to which a satellite can approach without breaking up depends on the rigidity of the satellite. At one extreme, a completely rigid satellite will maintain its shape until tidal forces break it apart. At the other extreme, a highly fluid satellite gradually deforms leading to increased tidal forces, causing the satellite to elongate, further compounding the tidal forces and causing it to break apart more readily.

Most real satellites would lie somewhere between these two extremes, with tensile strength rendering the satellite neither perfectly rigid nor perfectly fluid. For example, a rubble-pile asteroid will behave more like a fluid than a solid rocky one; an icy body will behave quite rigidly at first but become more fluid as tidal heating accumulates and its ices begin to melt.

But note that, as defined above, the Roche limit refers to a body held together solely by the gravitational forces which cause otherwise unconnected particles to coalesce, thus forming the body in question. The Roche limit is also usually calculated for the case of a circular orbit, although it is straightforward to modify the calculation to apply to the case (for example) of a body passing the primary on a parabolic or hyperbolic trajectory.

Rigid satellites

The rigid-body Roche limit is a simplified calculation for a spherical satellite. Irregular shapes such as those of tidal deformation on the body or the primary it orbits are neglected. It is assumed to be in hydrostatic equilibrium. These assumptions, although unrealistic, greatly simplify calculations.

The Roche limit for a rigid spherical satellite is the distance, ${\displaystyle d}$, from the primary at which the gravitational force on a test mass at the surface of the object is exactly equal to the tidal force pulling the mass away from the object:^[3][4]

${\displaystyle d=R_{M}\left(2{\frac {\rho _{M}}{\rho _{m}}}\right)^{\frac {1}{3}}}$

where ${\displaystyle R_{M}}$ is the radius of the primary, ${\displaystyle \rho _{M}}$ is the density of the primary, and ${\displaystyle \rho _{m}}$ is the density of the satellite. This can be equivalently written as

${\displaystyle d=R_{m}\left(2{\frac {M_{M}}{M_{m}}}\right)^{\frac {1}{3}}}$

where ${\displaystyle R_{m}}$ is the radius of the secondary, ${\displaystyle M_{M}}$ is the mass of the primary, and ${\displaystyle M_{m}}$ is the mass of the secondary. A third equivalent form uses only one property for each of the two bodies, the mass of the primary and the density of the secondary, is

${\displaystyle d=0.7816\left({\frac {M_{M}}{\rho _{m}}}\right)^{\frac {1}{3}}}$

These all represent the orbital distance inside of which loose material (e.g. regolith) on the surface of the satellite closest to the primary would be pulled away, and likewise material on the side opposite the primary will also go away from, rather than toward, the satellite.

Fluid satellites

A more accurate approach for calculating the Roche limit takes the deformation of the satellite into account. An extreme example would be a tidally locked liquid satellite orbiting a planet, where any force acting upon the satellite would deform it into a prolate spheroid.

The calculation is complex and its result cannot be represented in an exact algebraic formula. Roche himself derived the following approximate solution for the Roche limit:

${\displaystyle d\approx 2.44R\left({\frac {\rho _{M}}{\rho _{m}}}\right)^{1/3}}$

However, a better approximation that takes into account the primary's oblateness and the satellite's mass is:

${\displaystyle d\approx 2.423R\left({\frac {\rho _{M}}{\rho _{m}}}\right)^{1/3}\left({\frac {(1+{\frac {m}{3M}})+{\frac {c}{3R}}(1+{\frac {m}{M}})}{1-c/R}}\right)^{1/3}}$

where ${\displaystyle c/R}$ is the oblateness of the primary.

The fluid solution is appropriate for bodies that are only loosely held together, such as a comet. For instance, comet Shoemaker–Levy 9's decaying orbit around Jupiter passed within its Roche limit in July 1992, causing it to fragment into a number of smaller pieces. On its next approach in 1994 the fragments crashed into the planet. Shoemaker–Levy 9 was first observed in 1993, but its orbit indicated that it had been captured by Jupiter a few decades prior.^[5]

See also

• Roche lobe
• Chandrasekhar limit
• Spaghettification (the extreme case of tidal distortion)
• Hill sphere
• Sphere of influence (black hole)
• Black hole
• Triton (moon) (Neptune's satellite)
• Comet Shoemaker–Levy 9

References

1. Weisstein, Eric W. (2007). "Eric Weisstein's World of Physics – Roche Limit". scienceworld.wolfram.com. Retrieved September 5, 2007.
2. NASA. "What is the Roche limit?". NASA – JPL. Archived from the original on April 23, 2009. Retrieved September 5, 2007.
3. see calculation in Frank H. Shu, The Physical Universe: an Introduction to Astronomy, p. 431, University Science Books (1982), ISBN 0-935702-05-9.
4. "Roche Limit: Why Do Comets Break Up?". Archived from the original on 2013-05-15. Retrieved 2012-08-28.
5. International Planetarium Society Conference, Astronaut Memorial Planetarium & Observatory, Cocoa, Florida Rob Landis 10–16 July 1994 archive 21/12/1996

Sources

• Roche, Édouard (1849). "La figure d'une masse fluide soumise à l'attraction d'un point éloigné, part 1". Mémoires de la section des sciences, Volume 1. Académie des sciences de Montpellier. pp. 243–262. 2.44 is mentioned on page 258.
• Roche, Édouard (1850). "La figure d'une masse fluide soumise à l'attraction d'un point éloigné, part 2". Mémoires de la section des sciences, Volume 1. Académie des sciences de Montpellier. pp. 333–348.
• Roche, Édouard (1851). "La figure d'une masse fluide soumise à l'attraction d'un point éloigné, part 3". Mémoires de la section des sciences, Volume 2. Académie des sciences de Montpellier. pp. 21–32.
• Howard Darwin, George (1910). "On the figure and stability of a liquid satellite". Scientific Papers, Volume 3. pp. 436–524.
• Hopwood Jeans, James (1919). "Chapter III: Ellipsoidal configurations of equilibrium". Problems of cosmogony and stellar dynamics.
• Chandrasekhar, Subrahmanyan (1969). Ellipsoidal Figures of Equilibrium. Yale University Press. ISBN 978-0-300-01116-6.
• Chandrasekhar, S. (1963). "The Equilibrium and the Stability of the Roche Ellipsoids". The Astrophysical Journal. 138: 1182. Bibcode:1963ApJ...138.1182C. doi:10.1086/147716. ISSN 0004-637X.

External links

• Discussion of the Roche Limit; Archived 2019-09-16 at the Wayback Machine
• Audio: Cain/Gay – Astronomy Cast Tidal Forces Across the Universe – August 2007
• Roche Limit Description from NASA