vector confusion

[tony873004]

I'm trying to compute Mean Anomoly. Mean Anomoly is an angle that describes where in an orbit an object is relative to its periapsis. The formula according to Wikipedia is


M = E - e \cdot \sin E

where e is eccentricity (which I know), and E is Eccentric Anomoly.

According to Wikipedia, Eccentric Anomoly is

E = \arccos \frac{{1 - \left| r \right|/a}}{e}

where a is Semi-Major Axis (which I know), e is eccentricity (which I know), and r is an orbiting body's position vector. If I solve for r, I'm home free.

According to Wikipedia, The orbital position vector r is a cartesian vector describing the position of the orbiting body. Wouldn't that mean that r would be express as something like 1.0i + 2.0j+3.0k? But I can't plug something like that into the formula for Eccentric Anomoly. I could use Pothagorean Theorum to solve for distance and use this number. But that turns the vector into a scalar, and I doubt that's the right way to do it. Direction is pretty important here.

I know the object's x, y, and z position wrt the reference frame. How do I turn r into something I can use in these formulas?

[neutrino]

The formula involves only the modulus of the vector r, doesn't it?

[tony873004]

Modulus = absolute value??

In my example with 1.0i + 2.0j + 3.0k, I could do r=sqrt(1^2+2^2+3^2). But there are two points on the orbit that would have this same value for r. So I wouldn't know which one I computed.

[neutrino]

Modulus = absolute value??
Yes.


In my example with 1.0i + 2.0j + 3.0k, I could do r=sqrt(1^2+2^2+3^2). But there are two points on the orbit that would have this same value for r. So I wouldn't know which one I computed.
IIRC, you are the author of an orbit simulation program, right? I'm a novice when it comes at programming, so I don't understand the exact nature of your problem. Sorry. :redface:

[tony873004]

Yes :biggrin: . And if you use the program, you'll notice on the orbital elements box I leave out Mean Anomoly, simply because I don't get it right. I see many references that give the same formulas as Wikipedia for Mean Anomoly. And they all have the variable r in them. r is a vector, not a scalar, which is why I'm confused as to how to turn an x,y,& z position into a single number that I can assign to r that conveys both distance and direction. From physics classes, I remember that any answer that is a vector is stated as a scalar plus either an angle, or with the ijk-hat method. But of course any programming language doesn't want to see hats in the code. And E=Arcos((1-ABS(15, northwest)/a)/(e)) will generate a syntax error.

Thanks for your help thus far :smile:

[neutrino]

I have used your program before, and had fun generating all those patterns. :biggrin: But to fully appreciate a program such as this, I think I will need a decent understanding of celestial mechancis (I know it's not a necessity, but still I prefer it that way :) ). Keep up the good work, and I hope you get this problem solved.

[FrogPad]

I could be wrong here, because I have no clue about oribtal mechanics (if that's what it's called :smile:)

But, maybe this will help:
So you are trying to calculuate E

Defined (http://en.wikipedia.org/wiki/Eccentric_anomaly)by the following:

E = cos^{-1} \frac{1-\frac{| \vec r |}{a}}{e}

Looking up the definition of r and e we have:

Orbital Postion Vector (http://en.wikipedia.org/wiki/Orbital_position_vector):
\vec r

Since you are taking the modulus of this, you will return a scaler:
ie) | \vec r | = \sqrt{x^2+y^2+z^2}

This is the length of the vector. So assuming my geometry is correct (I haven't really worked with ellipses), you will have at least two spots where | \vec r | can be equal. For example if the ellipse was on 2d plane.

| \vec r_1 | = |\vec r_2 |
where:
\vec r_1 = (a,0,0)
\vec r_2 = (-a,0,0)

However, you are worried about a point on an ellipse, so you need some more information to make the angle unique (since \vec r by itself is not doing it).

Now if we look at e ,

Orbital Eccentricity (http://en.wikipedia.org/wiki/Orbital_eccentricity) ( e )

e = | \vec e |
where:

Eccentricity Vector (http://en.wikipedia.org/wiki/Eccentricity_vector)( \vec e )

\vec e = \frac{\vec v \times \vec h}{\vec \mu}-\frac{\vec r}{| \vec r |}
where:
\vec v = orbital velocity vector
\vec h = orbital angular momentum
\vec r = orbital position vector
\vec \mu = standard gravitational parameter

It would seem that at the point in question, \vec v would be unique, thus causing e = | \vec e | to be the unique quanitity that is dependent on position.

:blushing: Like I said, I could be way off here.

EDIT: I don't know what's up with the LaTeX... I guess I have an error somewhere. I hope this is somewhat readable.

[tony873004]

The LaTeX is fine. It doesn't work in preview mode though. Thanks. I think I'm getting a grip on it now. Using
| \vec r | = \sqrt{x^2+y^2+z^2}

I'm getting good results. But I would expect the angle to increase from 0 to 2pi over the course of an orbit. Instead, it increases from 0 to pi and then back to 0. If I subtract this angle from 2pi anytime the object is in the 3rd or 4th quadrant (negative y value), then all is well.

It just seems from the referenced formulas that this type of a piecewise answer is not necessary. But since taking the absolute value of the vector will yield the same answer for two different positions, I guess it is.

One silly mistake I was making was forgetting that the angle is measured from periapsis (closest point) rather than as a longitude (angle from a fixed direction, usually the Vernal equinox). But in a circular orbit, where the only hint of eccentricity comes 5 places to the right of the decimal, this point is not well defined and it drifts all over the place, causing Mean Anomoly to do the same. Once given a little eccentricity, things begin to work a lot better.