Kepler's equation

For specific applications of Kepler's equation, see Kepler's laws of planetary motion.

Kepler's equation solutions for five different eccentricities between 0 and 1

In orbital mechanics, Kepler's equation relates various geometric properties of the orbit of a body subject to a central force.

It was derived by Johannes Kepler in 1609 in Chapter 60 of his Astronomia nova , ^{[1] [2]} and in book V of his Epitome of Copernican Astronomy (1621) Kepler proposed an iterative solution to the equation. ^{[3] [4]} This equation and its solution, however, first appeared in a 9th-century work by Habash al-Hasib al-Marwazi, which dealt with problems of parallax. ^{[5] [6] [7] [8]} The equation has played an important role in the history of both physics and mathematics, particularly classical celestial mechanics.

Equation

Kepler's equation is

${\displaystyle M=E-e\sin E}$

where ${\displaystyle M}$ is the mean anomaly, ${\displaystyle E}$ is the eccentric anomaly, and ${\displaystyle e}$ is the eccentricity.

The 'eccentric anomaly' ${\displaystyle E}$ is useful to compute the position of a point moving in a Keplerian orbit. As for instance, if the body passes the periastron at coordinates ${\displaystyle x=a(1-e)}$, ${\displaystyle y=0}$, at time ${\displaystyle t=t_{0}}$, then to find out the position of the body at any time, you first calculate the mean anomaly ${\displaystyle M}$ from the time and the mean motion ${\displaystyle n}$ by the formula ${\displaystyle M=n(t-t_{0})}$, then solve the Kepler equation above to get ${\displaystyle E}$, then get the coordinates from:

${\displaystyle {\begin{array}{lcl}x&=&a(\cos E-e)\\y&=&b\sin E\end{array}}}$

where ${\displaystyle a}$ is the semi-major axis, ${\displaystyle b}$ the semi-minor axis.

Kepler's equation is a transcendental equation because sine is a transcendental function, and it cannot be solved for ${\displaystyle E}$ algebraically. Numerical analysis and series expansions are generally required to evaluate ${\displaystyle E}$.

Alternate forms

There are several forms of Kepler's equation. Each form is associated with a specific type of orbit. The standard Kepler equation is used for elliptic orbits (${\displaystyle 0\leq e<1}$). The hyperbolic Kepler equation is used for hyperbolic trajectories (${\displaystyle e>1}$). The radial Kepler equation is used for linear (radial) trajectories (${\displaystyle e=1}$). Barker's equation is used for parabolic trajectories (${\displaystyle e=1}$).

When ${\displaystyle e=0}$, the orbit is circular. Increasing ${\displaystyle e}$ causes the circle to become elliptical. When ${\displaystyle e=1}$, there are four possibilities:

• a parabolic trajectory,
• a trajectory that goes back and forth along a line segment from the centre of attraction to a point at some distance away,
• a trajectory going in or out along an infinite ray emanating from the centre of attraction, with its speed going to zero with distance
• or a trajectory along a ray, but with speed not going to zero with distance.

A value of ${\displaystyle e}$ slightly above 1 results in a hyperbolic orbit with a turning angle of just under 180 degrees. Further increases reduce the turning angle, and as ${\displaystyle e}$ goes to infinity, the orbit becomes a straight line of infinite length.

Hyperbolic Kepler equation

The Hyperbolic Kepler equation is:

${\displaystyle M=e\sinh H-H}$

where ${\displaystyle H}$ is the hyperbolic eccentric anomaly. This equation is derived by redefining M to be the square root of −1 times the right-hand side of the elliptical equation:

${\displaystyle M=i\left(E-e\sin E\right)}$

(in which ${\displaystyle E}$ is now imaginary) and then replacing ${\displaystyle E}$ by ${\displaystyle iH}$.

Radial Kepler equations

The Radial Kepler equation for the case where the object does not have enough energy to escape is:

${\displaystyle t(x)=\pm {\biggr [}\sin ^{-1}({\sqrt {x}})-{\sqrt {x(1-x)}}{\biggr ]}}$

where ${\displaystyle t}$ is proportional to time and ${\displaystyle x}$ is proportional to the distance from the centre of attraction along the ray and attains the value 1 at the maximum distance. This equation is derived by multiplying Kepler's equation by 1/2 and setting ${\displaystyle e}$ to 1:

${\displaystyle t(x)={\frac {1}{2}}\left[E-\sin E\right].}$

and then making the substitution

${\displaystyle E=2\sin ^{-1}({\sqrt {x}}).}$

The radial equation for when the object has enough energy to escape is:

${\displaystyle t(x)=\pm {\biggr [}\sinh ^{-1}({\sqrt {x}})-{\sqrt {x(1+x)}}{\biggr ]}}$

When the energy is exactly the minimum amount needed to escape, then the time is simply proportional to the distance to the power 3/2.

Inverse problem

Calculating ${\displaystyle M}$ for a given value of ${\displaystyle E}$ is straightforward. However, solving for ${\displaystyle E}$ when ${\displaystyle M}$ is given can be considerably more challenging. There is no closed-form solution. Solving for ${\displaystyle E}$ is more or less equivalent to solving for the true anomaly, or the difference between the true anomaly and the mean anomaly, which is called the "Equation of the center".

One can write an infinite series expression for the solution to Kepler's equation using Lagrange inversion, but the series does not converge for all combinations of ${\displaystyle e}$ and ${\displaystyle M}$ (see below).

Confusion over the solvability of Kepler's equation has persisted in the literature for four centuries. ^[9] Kepler himself expressed doubt at the possibility of finding a general solution:

I am sufficiently satisfied that it [Kepler's equation] cannot be solved a priori, on account of the different nature of the arc and the sine. But if I am mistaken, and any one shall point out the way to me, he will be in my eyes the great Apollonius.

— Johannes Kepler ^[10]

Fourier series expansion (with respect to ${\displaystyle M}$) using Bessel functions is ^{[11] [12] [13]}

${\displaystyle E=M+\sum _{m=1}^{\infty }{\frac {2}{m}}J_{m}(me)\sin(mM),\quad e\leq 1,\quad M\in [-\pi ,\pi ].}$

With respect to ${\displaystyle e}$, it is a Kapteyn series.

Inverse Kepler equation

The inverse Kepler equation is the solution of Kepler's equation for all real values of ${\displaystyle e}$:

${\displaystyle E={\begin{cases}\displaystyle \sum _{n=1}^{\infty }{\frac {M^{\frac {n}{3}}}{n!}}\lim _{\theta \to 0^{+}}\!{\Bigg (}{\frac {\mathrm {d} ^{\,n-1}}{\mathrm {d} \theta ^{\,n-1}}}{\bigg (}{\bigg (}{\frac {\theta }{\sqrt[{3}]{\theta -\sin(\theta )}}}{\bigg )}^{\!\!\!n}{\bigg )}{\Bigg )},&e=1\\\displaystyle \sum _{n=1}^{\infty }{\frac {M^{n}}{n!}}\lim _{\theta \to 0^{+}}\!{\Bigg (}{\frac {\mathrm {d} ^{\,n-1}}{\mathrm {d} \theta ^{\,n-1}}}{\bigg (}{\Big (}{\frac {\theta }{\theta -e\sin(\theta )}}{\Big )}^{\!n}{\bigg )}{\Bigg )},&e\neq 1\end{cases}}}$

Evaluating this yields:

${\displaystyle E={\begin{cases}\displaystyle s+{\frac {1}{60}}s^{3}+{\frac {1}{1400}}s^{5}+{\frac {1}{25200}}s^{7}+{\frac {43}{17248000}}s^{9}+{\frac {1213}{7207200000}}s^{11}+{\frac {151439}{12713500800000}}s^{13}+\cdots {\text{ with }}s=(6M)^{1/3},&e=1\\\\\displaystyle {\frac {1}{1-e}}M-{\frac {e}{(1-e)^{4}}}{\frac {M^{3}}{3!}}+{\frac {(9e^{2}+e)}{(1-e)^{7}}}{\frac {M^{5}}{5!}}-{\frac {(225e^{3}+54e^{2}+e)}{(1-e)^{10}}}{\frac {M^{7}}{7!}}+{\frac {(11025e^{4}+4131e^{3}+243e^{2}+e)}{(1-e)^{13}}}{\frac {M^{9}}{9!}}+\cdots ,&e\neq 1\end{cases}}}$

These series can be reproduced in Mathematica with the InverseSeries operation.

InverseSeries[Series[M-Sin[M],{M,0,10}]]

InverseSeries[Series[M-eSin[M],{M,0,10}]]

These functions are simple Maclaurin series. Such Taylor series representations of transcendental functions are considered to be definitions of those functions. Therefore, this solution is a formal definition of the inverse Kepler equation. However, ${\displaystyle E}$ is not an entire function of ${\displaystyle M}$ at a given non-zero ${\displaystyle e}$. Indeed, the derivative

${\displaystyle \mathrm {dM} /\mathrm {d} E=1-e\cos E}$

goes to zero at an infinite set of complex numbers when ${\displaystyle e<1,}$ the nearest to zero being at ${\displaystyle E=\pm i\cosh ^{-1}(1/e),}$ and at these two points

${\displaystyle M=E-e\sin E=\pm i\left(\cosh ^{-1}(1/e)-{\sqrt {1-e^{2}}}\right)}$

(where inverse cosh is taken to be positive), and ${\displaystyle \mathrm {d} E/\mathrm {d} M}$ goes to infinity at these values of ${\displaystyle M}$. This means that the radius of convergence of the Maclaurin series is ${\displaystyle \cosh ^{-1}(1/e)-{\sqrt {1-e^{2}}}}$ and the series will not converge for values of ${\displaystyle M}$ larger than this. The series can also be used for the hyperbolic case, in which case the radius of convergence is ${\displaystyle \cos ^{-1}(1/e)-{\sqrt {e^{2}-1}}.}$ The series for when ${\displaystyle e=1}$ converges when ${\displaystyle M<2\pi }$.

While this solution is the simplest in a certain mathematical sense,^{[ which? ]}, other solutions are preferable for most applications. Alternatively, Kepler's equation can be solved numerically.

The solution for ${\displaystyle e\neq 1}$ was found by Karl Stumpff in 1968, ^[14] but its significance wasn't recognized. ^{[15] [ clarification needed ]}

One can also write a Maclaurin series in ${\displaystyle e}$. This series does not converge when ${\displaystyle e}$ is larger than the Laplace limit (about 0.66), regardless of the value of ${\displaystyle M}$ (unless ${\displaystyle M}$ is a multiple of 2π), but it converges for all ${\displaystyle M}$ if ${\displaystyle e}$ is less than the Laplace limit. The coefficients in the series, other than the first (which is simply ${\displaystyle M}$), depend on ${\displaystyle M}$ in a periodic way with period 2π.

Inverse radial Kepler equation

The inverse radial Kepler equation (${\displaystyle e=1}$) for the case in which the object does not have enough energy to escape can similarly be written as:

${\displaystyle x(t)=\sum _{n=1}^{\infty }\left[\lim _{r\to 0^{+}}\left({\frac {t^{{\frac {2}{3}}n}}{n!}}{\frac {\mathrm {d} ^{\,n-1}}{\mathrm {d} r^{\,n-1}}}\!\left(r^{n}\left({\frac {3}{2}}{\Big (}\sin ^{-1}({\sqrt {r}})-{\sqrt {r-r^{2}}}{\Big )}\right)^{\!-{\frac {2}{3}}n}\right)\right)\right]}$

Evaluating this yields:

${\displaystyle x(t)=p-{\frac {1}{5}}p^{2}-{\frac {3}{175}}p^{3}-{\frac {23}{7875}}p^{4}-{\frac {1894}{3031875}}p^{5}-{\frac {3293}{21896875}}p^{6}-{\frac {2418092}{62077640625}}p^{7}-\ \cdots \ {\bigg |}{p=\left({\tfrac {3}{2}}t\right)^{2/3}}}$

To obtain this result using Mathematica:

InverseSeries[Series[ArcSin[Sqrt[t]]-Sqrt[(1-t)t],{t,0,15}]]

Numerical approximation of inverse problem

Newton's method

For most applications, the inverse problem can be computed numerically by finding the root of the function:

${\displaystyle f(E)=E-e\sin(E)-M(t)}$

This can be done iteratively via Newton's method:

${\displaystyle E_{n+1}=E_{n}-{\frac {f(E_{n})}{f'(E_{n})}}=E_{n}-{\frac {E_{n}-e\sin(E_{n})-M(t)}{1-e\cos(E_{n})}}}$

Note that ${\displaystyle E}$ and ${\displaystyle M}$ are in units of radians in this computation. This iteration is repeated until desired accuracy is obtained (e.g. when ${\displaystyle f(E)}$ < desired accuracy). For most elliptical orbits an initial value of ${\displaystyle E_{0}=M(t)}$ is sufficient. For orbits with ${\displaystyle e>0.8}$, a initial value of ${\displaystyle E_{0}=\pi }$ can be used. Numerous works developed accurate (but also more complex) start guesses. ^[16] If ${\displaystyle e}$ is identically 1, then the derivative of ${\displaystyle f}$, which is in the denominator of Newton's method, can get close to zero, making derivative-based methods such as Newton-Raphson, secant, or regula falsi numerically unstable. In that case, the bisection method will provide guaranteed convergence, particularly since the solution can be bounded in a small initial interval. On modern computers, it is possible to achieve 4 or 5 digits of accuracy in 17 to 18 iterations. ^[17] A similar approach can be used for the hyperbolic form of Kepler's equation. ^{[18] : 66–67} In the case of a parabolic trajectory, Barker's equation is used.

Fixed-point iteration

A related method starts by noting that ${\displaystyle E=M+e\sin {E}}$. Repeatedly substituting the expression on the right for the ${\displaystyle E}$ on the right yields a simple fixed-point iteration algorithm for evaluating ${\displaystyle E(e,M)}$. This method is identical to Kepler's 1621 solution. ^[4] In pseudocode:

functionE(e,M,n)E=Mfork=1tonE=M+e*sinEnextkreturnE

The number of iterations, ${\displaystyle n}$, depends on the value of ${\displaystyle e}$. The hyperbolic form similarly has ${\displaystyle H=\sinh ^{-1}\left({\frac {H+M}{e}}\right)}$.

This method is related to the Newton's method solution above in that

${\displaystyle E_{n+1}=E_{n}-{\frac {E_{n}-e\sin(E_{n})-M(t)}{1-e\cos(E_{n})}}=E_{n}+{\frac {(M+e\sin {E_{n}}-E_{n})(1+e\cos {E_{n}})}{1-e^{2}(\cos {E_{n}})^{2}}}}$

To first order in the small quantities ${\displaystyle M-E_{n}}$ and ${\displaystyle e}$,

${\displaystyle E_{n+1}\approx M+e\sin {E_{n}}}$.

See also

• Equation of the center
• Kepler's laws of planetary motion
• Kepler problem
• Kepler problem in general relativity
• Radial trajectory

References

1. Kepler, Johannes (1609). "LX. Methodus, ex hac Physica, hoc est genuina & verissima hypothesi, extruendi utramque partem æquationis, & distantias genuinas: quorum utrumque simul per vicariam fieri hactenus non potuit. argumentum falsæ hypotheseos". Astronomia Nova Aitiologētos, Seu Physica Coelestis, tradita commentariis De Motibus Stellæ Martis, Ex observationibus G. V. Tychonis Brahe (in Latin). pp. 299–300.
2. Aaboe, Asger (2001). Episodes from the Early History of Astronomy. Springer. pp. 146–147. ISBN   978-0-387-95136-2.
3. Kepler, Johannes (1621). "Libri V. Pars altera.". Epitome astronomiæ Copernicanæ usitatâ formâ Quæstionum & Responsionum conscripta, inq; VII. Libros digesta, quorum tres hi priores sunt de Doctrina Sphæricâ (in Latin). pp. 695–696.
4. Swerdlow, Noel M. (2000). "Kepler's Iterative Solution to Kepler's Equation". Journal for the History of Astronomy . 31 (4): 339–341. Bibcode:2000JHA....31..339S. doi:10.1177/002182860003100404. S2CID   116599258.
5. Colwell, Peter (1993). Solving Kepler's Equation Over Three Centuries. Willmann-Bell. p. 4. ISBN   978-0-943396-40-8.
6. Dutka, J. (1997-07-01). "A note on "Kepler's equation"". Archive for History of Exact Sciences. 51 (1): 59–65. Bibcode:1997AHES...51...59D. doi:10.1007/BF00376451. S2CID   122568981.
7. North, John (2008-07-15). Cosmos: An Illustrated History of Astronomy and Cosmology. University of Chicago Press. ISBN   978-0-226-59441-5.
8. Livingston, John W. (2017-12-14). The Rise of Science in Islam and the West: From Shared Heritage to Parting of The Ways, 8th to 19th Centuries. Routledge. ISBN   978-1-351-58926-0.
9. It is often claimed that Kepler's equation "cannot be solved analytically"; see for example here. Other authors claim that it cannot be solved at all; see for example Madabushi V. K. Chari; Sheppard Joel Salon; Numerical Methods in Electromagnetism, Academic Press, San Diego, CA, USA, 2000, ISBN   0-12-615760-X, p. 659
10. "Mihi ſufficit credere, ſolvi a priori non poſſe, propter arcus & ſinus ετερογενειαν. Erranti mihi, quicumque viam monſtraverit, is erit mihi magnus Apollonius." Hall, Asaph (May 1883). "Kepler's Problem". Annals of Mathematics. 10 (3): 65–66. doi:10.2307/2635832. JSTOR   2635832.
11. Fitzpatrick, Philip Matthew (1970). Principles of celestial mechanics. Academic Press. ISBN   0-12-257950-X.
12. Colwell, Peter (January 1992). "Bessel Functions and Kepler's Equation". The American Mathematical Monthly. 99 (1): 45–48. doi:10.2307/2324547. ISSN   0002-9890. JSTOR   2324547.
13. Boyd, John P. (2007). "Rootfinding for a transcendental equation without a first guess: Polynomialization of Kepler's equation through Chebyshev polynomial equation of the sine". Applied Numerical Mathematics. 57 (1): 12–18. doi:10.1016/j.apnum.2005.11.010.
14. Stumpff, Karl (1 June 1968). "On The application of Lie-series to the problems of celestial mechanics". NASA Technical Note D-4460.{{cite journal}}: Cite journal requires |journal= (help)
15. Colwell, Peter (1993). Solving Kepler's Equation Over Three Centuries. Willmann–Bell. p. 43. ISBN   0-943396-40-9.
16. Odell, A. W.; Gooding, R. H. (1986). "Procedures for solving Kepler's equation". Celestial Mechanics. 38 (4). Springer Science and Business Media LLC: 307–334. Bibcode:1986CeMec..38..307O. doi:10.1007/bf01238923. ISSN   1572-9478. S2CID   120179781.
17. Keister, Adrian. "The Numerical Analysis of Finding the Height of a Circular Segment". Wineman Technology. Wineman Technology, Inc. Retrieved 28 December 2019.
18. Pfleger, Thomas; Montenbruck, Oliver (1998). Astronomy on the Personal Computer (Third ed.). Berlin, Heidelberg: Springer. ISBN   978-3-662-03349-4.

External links

• Danby, John M.; Burkardt, Thomas M. (1983). "The solution of Kepler's equation. I". Celestial Mechanics. 31 (2): 95–107. Bibcode:1983CeMec..31...95D. doi:10.1007/BF01686811. S2CID   189832421.
• Conway, Bruce A. (1986). "An improved algorithm due to Laguerre for the solution of Kepler's equation". 24th Aerospace Sciences Meeting. doi:10.2514/6.1986-84.
• Mikkola, Seppo (1987). "A cubic approximation for Kepler's equation" (PDF). Celestial Mechanics. 40 (3): 329–334. Bibcode:1987CeMec..40..329M. doi:10.1007/BF01235850. S2CID   122237945.
• Nijenhuis, Albert (1991). "Solving Kepler's equation with high efficiency and accuracy". Celestial Mechanics and Dynamical Astronomy. 51 (4): 319–330. Bibcode:1991CeMDA..51..319N. doi:10.1007/BF00052925. S2CID   121845017.
• Markley, F. Landis (1995). "Kepler equation solver". Celestial Mechanics and Dynamical Astronomy. 63 (1): 101–111. Bibcode:1995CeMDA..63..101M. doi:10.1007/BF00691917. S2CID   120405765.
• Fukushima, Toshio (1996). "A method solving kepler's equation without transcendental function evaluations". Celestial Mechanics and Dynamical Astronomy. 66 (3): 309–319. Bibcode:1996CeMDA..66..309F. doi:10.1007/BF00049384. S2CID   120352687.
• Charles, Edgar D.; Tatum, Jeremy B. (1997). "The convergence of Newton-Raphson iteration with Kepler's equation". Celestial Mechanics and Dynamical Astronomy. 69 (4): 357–372. Bibcode:1997CeMDA..69..357C. doi:10.1023/A:1008200607490. S2CID   118637706.
• Stumpf, Laura (1999). "Chaotic behaviour in the Newton iterative function associated with Kepler's equation". Celestial Mechanics and Dynamical Astronomy. 74 (2): 95–109. Bibcode:1999CeMDA..74...95S. doi:10.1023/A:1008339416143. S2CID   122491746.
• Palacios, Manuel (2002). "Kepler equation and accelerated Newton method". Journal of Computational and Applied Mathematics. 138 (2): 335–346. Bibcode:2002JCoAM.138..335P. doi: 10.1016/S0377-0427(01)00369-7 .
• Boyd, John P. (2007). "Rootfinding for a transcendental equation without a first guess: Polynomialization of Kepler's equation through Chebyshev polynomial equation of the sine". Applied Numerical Mathematics. 57 (1): 12–18. doi:10.1016/j.apnum.2005.11.010.
• Pál, András (2009). "An analytical solution for Kepler's problem". Monthly Notices of the Royal Astronomical Society. 396 (3): 1737–1742. arXiv: 0904.0324 . Bibcode:2009MNRAS.396.1737P. doi: 10.1111/j.1365-2966.2009.14853.x .
• Esmaelzadeh, Reza; Ghadiri, Hossein (2014). "Appropriate starter for solving the Kepler's equation". International Journal of Computer Applications. 89 (7): 31–38. Bibcode:2014IJCA...89g..31E. doi: 10.5120/15517-4394 .
• Zechmeister, Mathias (2018). "CORDIC-like method for solving Kepler's equation". Astronomy and Astrophysics. 619: A128. arXiv: 1808.07062 . Bibcode:2018A&A...619A.128Z. doi: 10.1051/0004-6361/201833162 .

• Kepler's Equation at Wolfram Mathworld