Jacobi integral

Jacobi constant, Zero Velocity Surface and Curve

In celestial mechanics, Jacobi's integral (also known as the Jacobi integral or Jacobi constant) is the only known conserved quantity for the circular restricted three-body problem. ^[1] Unlike in the two-body problem, the energy and momentum of the system are not conserved separately and a general analytical solution is not possible. The integral has been used to derive numerous solutions in special cases.

It was named after German mathematician Carl Gustav Jacob Jacobi.

Definition

Synodic system

Co-rotating system

One of the suitable coordinate systems used is the so-called synodic or co-rotating system, placed at the barycentre, with the line connecting the two masses μ₁, μ₂ chosen as x-axis and the length unit equal to their distance. As the system co-rotates with the two masses, they remain stationary and positioned at (−μ₂, 0) and (+μ₁, 0). ^{[lower-alpha 1]}

In the (x, y)-coordinate system, the Jacobi constant is expressed as follows:

${\displaystyle C_{J}=n^{2}\left(x^{2}+y^{2}\right)+2\left({\frac {\mu _{1}}{r_{1}}}+{\frac {\mu _{2}}{r_{2}}}\right)-\left({\dot {x}}^{2}+{\dot {y}}^{2}+{\dot {z}}^{2}\right)}$

where:

• n = 2π/T is the mean motion (orbital period T)
• μ₁ = Gm₁, μ₂ = Gm₂, for the two masses m₁, m₂ and the gravitational constant  G
• r₁, r₂ are distances of the test particle from the two masses

Note that the Jacobi integral is minus twice the total energy per unit mass in the rotating frame of reference: the first term relates to centrifugal potential energy, the second represents gravitational potential and the third is the kinetic energy. In this system of reference, the forces that act on the particle are the two gravitational attractions, the centrifugal force and the Coriolis force. Since the first three can be derived from potentials and the last one is perpendicular to the trajectory, they are all conservative, so the energy measured in this system of reference (and hence, the Jacobi integral) is a constant of motion. For a direct computational proof, see below.

Sidereal system

Inertial system.

In the inertial, sidereal co-ordinate system (ξ, η, ζ), the masses are orbiting the barycentre. In these co-ordinates the Jacobi constant is expressed by ^[2]

${\displaystyle C_{J}=2\left({\frac {\mu _{1}}{r_{1}}}+{\frac {\mu _{2}}{r_{2}}}\right)+2n\left(\xi {\dot {\eta }}-\eta {\dot {\xi }}\right)-\left({\dot {\xi }}^{2}+{\dot {\eta }}^{2}+{\dot {\zeta }}^{2}\right).}$

Derivation

In the co-rotating system, the accelerations can be expressed as derivatives of a single scalar function

${\displaystyle U(x,y,z)={\frac {n^{2}}{2}}\left(x^{2}+y^{2}\right)+{\frac {\mu _{1}}{r_{1}}}+{\frac {\mu _{2}}{r_{2}}}}$

Using Lagrangian representation of the equations of motion:

${\displaystyle {\ddot {x}}-2n{\dot {y}}={\frac {\delta U}{\delta x}}}$

(1)

${\displaystyle {\ddot {y}}+2n{\dot {x}}={\frac {\delta U}{\delta y}}}$

(2)

${\displaystyle {\ddot {z}}={\frac {\delta U}{\delta z}}}$

(3)

Multiplying Eqs. ( 1 ), ( 2 ), and ( 3 ) by ẋ, ẏ and ż respectively and adding all three yields

${\displaystyle {\dot {x}}{\ddot {x}}+{\dot {y}}{\ddot {y}}+{\dot {z}}{\ddot {z}}={\frac {\delta U}{\delta x}}{\dot {x}}+{\frac {\delta U}{\delta y}}{\dot {y}}+{\frac {\delta U}{\delta z}}{\dot {z}}={\frac {dU}{dt}}}$

Integrating yields

${\displaystyle {\dot {x}}^{2}+{\dot {y}}^{2}+{\dot {z}}^{2}=2U-C_{J}}$

where C_J is the constant of integration.

The left side represents the square of the velocity v of the test particle in the co-rotating system.

See also

• Rotating reference frame
• Tisserand's criterion
• Zero velocity surface

Notes

1. This coordinate system is non-inertial, which explains the appearance of terms related to centrifugal and Coriolis accelerations.

1. Bibliothèque nationale de France. Jacobi, Carl G. J. (1836). "Sur le movement d'un point et sur un cas particulier du problème des trois corps". Comptes Rendus de l'Académie des Sciences de Paris. 3: 59–61.
2. Murray, Carl D.; Dermott, Stanley F. (1999). Solar System Dynamics (1st ed.). Cambridge University Press. pp. 66–70. ISBN   9780521575973.

Bibliography

• Carl D. Murray and Stanley F. Dermot Solar System Dynamics [Cambridge, England: Cambridge University Press, 1999], pages 68–71. ( ISBN   0-521-57597-4)