- Source: Jacobi integral
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. Unlike in the two-body problem, the energy and momentum of each the system bodies comprising the system are not conserved separately, and a general analytical solution is not possible. With the gravitational force being conservative, the total energy (hamiltonian), the linear moment and the angular momentum of an isolated three-body system (the problem being either restricted or not) are conserved.
It was named after German mathematician Carl Gustav Jacob Jacobi.
Definition
= Synodic 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).
In the (x, y)-coordinate system, the Jacobi constant is expressed as follows:
C
J
=
n
2
(
x
2
+
y
2
)
+
2
(
μ
1
r
1
+
μ
2
r
2
)
−
(
x
˙
2
+
y
˙
2
+
z
˙
2
)
{\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
=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
C
J
=
2
(
μ
1
r
1
+
μ
2
r
2
)
+
2
n
(
ξ
η
˙
−
η
ξ
˙
)
−
(
ξ
˙
2
+
η
˙
2
+
ζ
˙
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
U
(
x
,
y
,
z
)
=
n
2
2
(
x
2
+
y
2
)
+
μ
1
r
1
+
μ
2
r
2
{\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:
Multiplying Eqs. (1), (2), and (3) by ẋ, ẏ and ż respectively and adding all three yields
x
˙
x
¨
+
y
˙
y
¨
+
z
˙
z
¨
=
δ
U
δ
x
x
˙
+
δ
U
δ
y
y
˙
+
δ
U
δ
z
z
˙
=
d
U
d
t
{\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
x
˙
2
+
y
˙
2
+
z
˙
2
=
2
U
−
C
J
{\displaystyle {\dot {x}}^{2}+{\dot {y}}^{2}+{\dot {z}}^{2}=2U-C_{J}}
where CJ 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
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)
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