Equation giving the form of a central force
The Binet equation, derived by Jacques Philippe Marie Binet, provides the form of a central force given the shape of the orbital motion in plane polar coordinates. The equation can also be used to derive the shape of the orbit for a given force law, but this usually involves the solution to a second order nonlinear, ordinary differential equation. A unique solution is impossible in the case of circular motion about the center of force.
Equation
The shape of an orbit is often conveniently described in terms of relative distance
as a function of angle
. For the Binet equation, the orbital shape is instead more concisely described by the reciprocal
as a function of
. Define the specific angular momentum as
where
is the angular momentum and
is the mass. The Binet equation, derived in the next section, gives the force in terms of the function
:
![{\displaystyle F(u^{-1})=-mh^{2}u^{2}\left({\frac {\mathrm {d} ^{2}u}{\mathrm {d} \theta ^{2}}}+u\right).}](https://wikimedia.org/api/rest_v1/media/math/render/svg/9f31c97629c4f6ef6246b0cdd3ce1076ce272720)
Derivation
Newton's Second Law for a purely central force is
![{\displaystyle F(r)=m\left({\ddot {r}}-r{\dot {\theta }}^{2}\right).}](https://wikimedia.org/api/rest_v1/media/math/render/svg/a2cf97b4f5da84acc42864fff246f7b402cf2e5c)
The conservation of angular momentum requires that
![{\displaystyle r^{2}{\dot {\theta }}=h={\text{constant}}.}](https://wikimedia.org/api/rest_v1/media/math/render/svg/1df83bee8ce360aeb32069d6b5e034c4f135bcbf)
Derivatives of
with respect to time may be rewritten as derivatives of
with respect to angle:
![{\displaystyle {\begin{aligned}&{\frac {\mathrm {d} u}{\mathrm {d} \theta }}={\frac {\mathrm {d} }{\mathrm {d} t}}\left({\frac {1}{r}}\right){\frac {\mathrm {d} t}{\mathrm {d} \theta }}=-{\frac {\dot {r}}{r^{2}{\dot {\theta }}}}=-{\frac {\dot {r}}{h}}\\&{\frac {\mathrm {d} ^{2}u}{\mathrm {d} \theta ^{2}}}=-{\frac {1}{h}}{\frac {\mathrm {d} {\dot {r}}}{\mathrm {d} t}}{\frac {\mathrm {d} t}{\mathrm {d} \theta }}=-{\frac {\ddot {r}}{h{\dot {\theta }}}}=-{\frac {\ddot {r}}{h^{2}u^{2}}}\end{aligned}}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/3b6b4e660446697917e4fb163555f651175e27b3)
Combining all of the above, we arrive at
![{\displaystyle F=m\left({\ddot {r}}-r{\dot {\theta }}^{2}\right)=-m\left(h^{2}u^{2}{\frac {\mathrm {d} ^{2}u}{\mathrm {d} \theta ^{2}}}+h^{2}u^{3}\right)=-mh^{2}u^{2}\left({\frac {\mathrm {d} ^{2}u}{\mathrm {d} \theta ^{2}}}+u\right)}](https://wikimedia.org/api/rest_v1/media/math/render/svg/914cbca590c97ac9418ded447dacf43d70b3072f)
The general solution is [1]
![{\displaystyle \theta =\int _{r_{0}}^{r}{\frac {\mathrm {d} r}{r^{2}{\sqrt {{\frac {2m}{L^{2}}}(E-V)-{\frac {1}{r^{2}}}}}}}+\theta _{0}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/d7b7c92fa70b778a21785f1fe537860a74855cd3)
where
![{\displaystyle (r_{0},\theta _{0})}](https://wikimedia.org/api/rest_v1/media/math/render/svg/081118f53768b7ba0aa01cb89676c270d0d5657a)
is the initial coordinate of the particle.
Examples
Kepler problem
Classical
The traditional Kepler problem of calculating the orbit of an inverse square law may be read off from the Binet equation as the solution to the differential equation
![{\displaystyle -ku^{2}=-mh^{2}u^{2}\left({\frac {\mathrm {d} ^{2}u}{\mathrm {d} \theta ^{2}}}+u\right)}](https://wikimedia.org/api/rest_v1/media/math/render/svg/9e6068c03ba1584dace0a6ae69df35c6a9ada583)
![{\displaystyle {\frac {\mathrm {d} ^{2}u}{\mathrm {d} \theta ^{2}}}+u={\frac {k}{mh^{2}}}\equiv {\text{constant}}>0.}](https://wikimedia.org/api/rest_v1/media/math/render/svg/9a9b8c38205413ab41746788d01f55841b293bad)
If the angle
is measured from the periapsis, then the general solution for the orbit expressed in (reciprocal) polar coordinates is
![{\displaystyle lu=1+\varepsilon \cos \theta .}](https://wikimedia.org/api/rest_v1/media/math/render/svg/0c4af9e72d02c6b380011b0d3553b0453ef51350)
The above polar equation describes conic sections, with
the semi-latus rectum (equal to
) and
the orbital eccentricity.
Relativistic
The relativistic equation derived for Schwarzschild coordinates is[2]
![{\displaystyle {\frac {\mathrm {d} ^{2}u}{\mathrm {d} \theta ^{2}}}+u={\frac {r_{s}c^{2}}{2h^{2}}}+{\frac {3r_{s}}{2}}u^{2}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/0c68791c117ca558900ed9fc3f02b828206bb26e)
where
![{\displaystyle c}](https://wikimedia.org/api/rest_v1/media/math/render/svg/86a67b81c2de995bd608d5b2df50cd8cd7d92455)
is the
speed of light and
![{\displaystyle r_{s}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/28528468fc3b17c72144f4ba50bb7b4257c1e316)
is the
Schwarzschild radius. And for
Reissner–Nordström metric we will obtain
![{\displaystyle {\frac {\mathrm {d} ^{2}u}{\mathrm {d} \theta ^{2}}}+u={\frac {r_{s}c^{2}}{2h^{2}}}+{\frac {3r_{s}}{2}}u^{2}-{\frac {GQ^{2}}{4\pi \varepsilon _{0}c^{4}}}\left({\frac {c^{2}}{h^{2}}}u+2u^{3}\right)}](https://wikimedia.org/api/rest_v1/media/math/render/svg/9faa92651b9b454465a9d213311fabca64a9711f)
where
![{\displaystyle Q}](https://wikimedia.org/api/rest_v1/media/math/render/svg/8752c7023b4b3286800fe3238271bbca681219ed)
is the
electric charge and
![{\displaystyle \varepsilon _{0}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/acb0a8377db20e42274444cb181d51b5532b5844)
is the
vacuum permittivity.
Inverse Kepler problem
Consider the inverse Kepler problem. What kind of force law produces a noncircular elliptical orbit (or more generally a noncircular conic section) around a focus of the ellipse?
Differentiating twice the above polar equation for an ellipse gives
![{\displaystyle l\,{\frac {\mathrm {d} ^{2}u}{\mathrm {d} \theta ^{2}}}=-\varepsilon \cos \theta .}](https://wikimedia.org/api/rest_v1/media/math/render/svg/7d23a86a705ed47cdefacf97f903c6a06e5ff4c8)
The force law is therefore
![{\displaystyle F=-mh^{2}u^{2}\left({\frac {-\varepsilon \cos \theta }{l}}+{\frac {1+\varepsilon \cos \theta }{l}}\right)=-{\frac {mh^{2}u^{2}}{l}}=-{\frac {mh^{2}}{lr^{2}}},}](https://wikimedia.org/api/rest_v1/media/math/render/svg/83e527395aaa9848ae017d5cc177ed24d3560e69)
which is the anticipated inverse square law. Matching the orbital
![{\displaystyle h^{2}/l=\mu }](https://wikimedia.org/api/rest_v1/media/math/render/svg/06594bc11d46a283520cde4e6f4ee889425399d1)
to physical values like
![{\displaystyle GM}](https://wikimedia.org/api/rest_v1/media/math/render/svg/d2d9b5427dc6e6f3c11f13d88a5b637b4bc24585)
or
![{\displaystyle k_{e}q_{1}q_{2}/m}](https://wikimedia.org/api/rest_v1/media/math/render/svg/b7e580ddbb07785521e16825aa4d6ee525b7ea31)
reproduces
Newton's law of universal gravitation or
Coulomb's law, respectively.
The effective force for Schwarzschild coordinates is[3]
![{\displaystyle F=-GMmu^{2}\left(1+3\left({\frac {hu}{c}}\right)^{2}\right)=-{\frac {GMm}{r^{2}}}\left(1+3\left({\frac {h}{rc}}\right)^{2}\right).}](https://wikimedia.org/api/rest_v1/media/math/render/svg/22d06532b635a3f549c31b63c0777dc333c8dbbe)
where the second term is an inverse-quartic force corresponding to quadrupole effects such as the angular shift of
periapsis (It can be also obtained via retarded potentials
[4]).
In the parameterized post-Newtonian formalism we will obtain
![{\displaystyle F=-{\frac {GMm}{r^{2}}}\left(1+(2+2\gamma -\beta )\left({\frac {h}{rc}}\right)^{2}\right).}](https://wikimedia.org/api/rest_v1/media/math/render/svg/b50d8105763491668cc41d5fbeeb5339da5b287e)
where
![{\displaystyle \gamma =\beta =1}](https://wikimedia.org/api/rest_v1/media/math/render/svg/fb96b68c1387c6ca1938c729d89302b6cdd5ceb4)
for the
general relativity and
![{\displaystyle \gamma =\beta =0}](https://wikimedia.org/api/rest_v1/media/math/render/svg/5f78a04841def5094970d96aecaa98897581b8a5)
in the classical case.
Cotes spirals
An inverse cube force law has the form
![{\displaystyle F(r)=-{\frac {k}{r^{3}}}.}](https://wikimedia.org/api/rest_v1/media/math/render/svg/e2108eeb25d2aeba5de784d56c698d44c4944e23)
The shapes of the orbits of an inverse cube law are known as Cotes spirals. The Binet equation shows that the orbits must be solutions to the equation
![{\displaystyle {\frac {\mathrm {d} ^{2}u}{\mathrm {d} \theta ^{2}}}+u={\frac {ku}{mh^{2}}}=Cu.}](https://wikimedia.org/api/rest_v1/media/math/render/svg/041d335b8b7e21e74cc0b914f9a2290d53c4e926)
The differential equation has three kinds of solutions, in analogy to the different conic sections of the Kepler problem. When
, the solution is the epispiral, including the pathological case of a straight line when
. When
, the solution is the hyperbolic spiral. When
the solution is Poinsot's spiral.
Off-axis circular motion
Although the Binet equation fails to give a unique force law for circular motion about the center of force, the equation can provide a force law when the circle's center and the center of force do not coincide. Consider for example a circular orbit that passes directly through the center of force. A (reciprocal) polar equation for such a circular orbit of diameter
is
![{\displaystyle D\,u(\theta )=\sec \theta .}](https://wikimedia.org/api/rest_v1/media/math/render/svg/92c81bbd10f136088e8589c593bcb4b4452f3e32)
Differentiating
twice and making use of the Pythagorean identity gives
![{\displaystyle D\,{\frac {\mathrm {d} ^{2}u}{\mathrm {d} \theta ^{2}}}=\sec \theta \tan ^{2}\theta +\sec ^{3}\theta =\sec \theta (\sec ^{2}\theta -1)+\sec ^{3}\theta =2D^{3}u^{3}-D\,u.}](https://wikimedia.org/api/rest_v1/media/math/render/svg/03011872fd584c1e072961026165ca68feb99ad6)
The force law is thus
![{\displaystyle F=-mh^{2}u^{2}\left(2D^{2}u^{3}-u+u\right)=-2mh^{2}D^{2}u^{5}=-{\frac {2mh^{2}D^{2}}{r^{5}}}.}](https://wikimedia.org/api/rest_v1/media/math/render/svg/7b6490c1a48b9bfa5a3f82eec1b5b621145110c2)
Note that solving the general inverse problem, i.e. constructing the orbits of an attractive
force law, is a considerably more difficult problem because it is equivalent to solving
![{\displaystyle {\frac {\mathrm {d} ^{2}u}{\mathrm {d} \theta ^{2}}}+u=Cu^{3}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/808f516089eb7b6200289aee54794c880071b85c)
which is a second order nonlinear differential equation.
See also
Astronomy portal
Physics portal
References
- ^ Goldstein, Herbert (1980). Classical mechanics. Reading, Mass.: Addison-Wesley Pub. Co. ISBN 0-201-02918-9. OCLC 5675073.
- ^ "Archived copy" (PDF). Archived from the original (PDF) on 2010-06-19. Retrieved 2010-11-15.
{{cite web}}
: CS1 maint: archived copy as title (link) - ^ http://chaos.swarthmore.edu/courses/PDG07/AJP/AJP000352.pdf - The first-order orbital equation
- ^ Behera, Harihar; Naik, P. C (2003). "A flat space-time relativistic explanation for the perihelion advance of Mercury". arXiv:astro-ph/0306611.