Calculating time until apoapsis analytically

[Greg Bernhardt]

Definition/Summary

The furthest point of an elliptical orbit from the focus of the orbit

Equations

r_A = a(1+e)

where:
a is the semi-major axis
e is the eccentricity

Extended explanation

The apoapsis is one of two apsides that are located on the points where a line passing through the focus and bisecting the ellipse along its long dimension intersects the orbit.

The line passing through the two apsides is known as the Line of Apsides.

The segment of the line of apsides that lies between the apsides is the Major Axis of the orbit, and half of this is the Semi-major Axis (a).

For a Sun centered orbit, the apoapsis is called the aphelion and for an Earth centered orbit its is called the apogee. Each major body of the Solar system also has its own specifically named apoapsis.

* This entry is from our old Library feature. If you know who wrote it, please let us know so we can attribute a writer. Thanks!

 

[ellipsis]

Given general information about the current orbit (eccentricity, semi-major axis, apoapsis, etc), as well as positional information (position, velocity, true anomaly) I would like to calculate the time until the smaller body reaches the apoapsis of its orbit. This is a restricted two-body problem, in that the mass of the smaller body is negligibly small.

I have a suspicion that I can use the true anomaly somehow to calculate time between points. However, I cannot find a reference online for it, and I have no idea how to derive it.

I can calculate the orbital period, though, and I know that the orbit of anybody sweeps out the same amount of area each equal time interval. I could maybe find a formula to find the area of an arc on an ellipse, then divide that quantity by the total area, then multiply by the orbital period.

It's funny how simply writing out a post comprehensively helps you think better about how to solve a problem. That is probably not a possible way to derive it, though, so you guys tell me how anyway.

 

[D H]

I have a suspicion that I can use the true anomaly somehow to calculate time between points.

Five easy steps:

1. Calculate the eccentric anomaly E from the true anomaly \theta via
   \tan\frac E 2 \sqrt{\frac{1-e}{1+e}} \tan \frac \theta 2
   Note that this will yield a value between -pi and pi if you use the standard definition of arc tangent.
2. Calculate the mean anomaly M from the eccentric anomaly E via Kepler's equation,
   M = E - e\sin E
3. Calculate the change in mean anomaly \Delta M from the calculated value of M to that at apoapsis, which is \pi:
   \Delta M = \pi - M
4. Calculate the mean motion m:
   n = \sqrt{\frac{GM}{a^3}}
5. Calculate time to apoapsis:
   \Delta t = \frac{\Delta M}{n}

 

[ellipsis]

Thank you so much... I will get to work on this immediately. (I am rather glad, since that derivation idea I had involved integration in polar coordinates, yuck)