Suppose you have a finite collection of point particles interacting gravitationally via good old Newtonian mechanics. And suppose that:

- The time averages of the total kinetic energy and the total potential energy are well-defined.
- The positions and velocities of the particles are bounded for all time.

<T> = -<V>/2where <T> is the time average of the total kinetic energy, and <V> is the time average of the total potential energy.

I always found this to be a bit magical. It seems surprising at first that such a simple law could hold so generally. But in fact, it's just a special case of something called the "virial theorem", which also applies to forces other than gravity, and impacts everything from astronomy to the theory of gases.

For example, out in space, very often a bunch of particles will collapse to form a gravitationally bound system. If the system is roughly in equilibrium so the time averages of kinetic and potential energy are close to their current values, the virial theorem implies that T = -(1/2) V. we know that <T> = -<V>/2. This is a terrific thing, because it lets you find the masses of bound systems. In fact, it's really the reason we think that dark matter exists.

To be specific, suppose you measure the speeds of a bunch of visible objects in your system, and infer T. Then the virial theorem tells you V. If you find out that the potential well is deeper than what you'd get by adding up the contributions from the masses of everything you see, you know there's dark matter. People do this for spiral galaxies, elliptical galaxies, and galaxy clusters, getting strong evidence for dark matter in all cases.

For applications of the virial theorem to astrophysics, this book is good:

- William C. Saslaw, Gravitational physics of stellar and galactic systems, Cambridge U. Press, Cambridge, 1985.

Before I sketch the proof of the virial theorem, let's consider the simplest possible case: a single light particle in circular orbit around a heavy one. Say the light one has mass m and the heavy one has mass M. And suppose the orbit has radius R. Then the potential energy is

V = -GmM/R (1)where G is Newton's constant. To figure out the kinetic energy, remember that the gravitational force is

Fwhile the centrifugal force is_{grav}= -GmM/R^{2}

FIn a circular orbit these counteract each other perfectly, so we must have_{centrif}= mv^{2}/R

mvThus the kinetic energy of the light particle is^{2}/R = GmM/R^{2}

T = mvwhile the kinetic energy of the heavy one is negligible. Comparing (1) and (2), we see that^{2}/2 = GmM/2R (2)

T = -V/2just as the virial theorem says!

The virial theorem lets us generalize this fact to arbitrary gravitationally bound systems. Of course, in a more general system of this sort - even a particle in an elliptical orbit - the kinetic and potential energy change with time. That's why the virial theorem refers to time averages of the kinetic and potential energy. But the basic idea is the same. And the proof is surprisingly simple.

Here's how it goes. We consider a quantity called the "virial":

G = ∑that is, the sum over all the particles of the dot product of each particle's momentum with its position. A little calculation shows that_{i}p_{i}^{.}r_{i}

dG/dt = 2T + ∑where F_{i}F_{i}^{.}r_{i}

limsince by assumption 2 the function G(t) is bounded. We thus obtain_{t -> ∞}(G(t) - G(0))/t = 0

0 = 2<T> + <∑at least if the time averages here are well-defined. We know that <T> is well-defined by assumption 1. Why is that other time average well-defined? Well, the force on the ith particle is caused by all the other particles, so we have_{i}F_{i}^{.}r_{i}>

∑where V_{i}F_{i}^{.}r_{i}= ∑_{i ≠ j}-grad(V_{ij})^{.}r_{i}

∑where in the second step we switched the dummy indices i and j on the second term. Now, since V_{i}F_{i}^{.}r_{i}= ∑_{i < j}-grad(V_{ij})^{.}r_{i}+ ∑_{j < i}-grad(V_{ij})^{.}r_{i}= ∑_{i < j}-grad(V_{ij})^{.}r_{i}+ ∑_{i < j}-grad(V_{ji})^{.}r_{j}= ∑_{i < j}-grad(V_{ij})^{.}(r_{i}- r_{j})

grad(Vso_{ij})^{.}(r_{i}- r_{j}) = - V_{ij}

<∑so this time average is well-defined by assumption 1. We also see what it equals! So we get_{i}F_{i}^{.}r_{i}> = <∑_{i < j}V_{ij}> = <V>

0 = 2<T> + <V>or in other words

<T> = -<V>/2Voila! The virial theorem!

You can find this proof in any good textbook on classical mechanics, for example:

- Herbert Goldstein, Classical Mechanics, Addison-Wesley, Reading, Massachusetts, 1950.

Having done all that work proving the virial theorem, it's nice to note some spinoffs.

First of all, if the motion of our particles is periodic, we don't need to average over all time: we can just average over a period. This applies to one particle in elliptical orbit about another, for example. You could also handle that case using Kepler's laws, but I like the greater generality of what we just did.

Also, the virial theorem can be adapted to some other forces! Suppose the potential between particles is proportional to the nth power of their distance. This only changes the above argument a little bit. We get

grad(Vso we get_{ij})^{.}(r_{i}- r_{j}) = n V_{ij}

<T> = (n/2) <V>.

With extra work, we can generalize the ideas behind the virial theorem to obtain useful results about other more complicated forces. This is especially important in the theory of gases, where we measure the deviation from being an ideal gas using "virial coefficients".

But finally, before you walk away feeling too happy, I should warn you that
in astrophysics,
assumption 2 is usually not quite true! For example, a galaxy will
occasionally fling stars into the vastness of space, making their position
unbounded as a function of
time. This process of "boiling off" is very important in the long
run, as explained in my webpage on the end of the
universe. But it's very slow, so the conditions of the virial
theorem seem to be "approximately true" in the short run. Most people
go ahead and use it without worrying about this subtlety. To justify
this, we should modify
the above argument by averaging not over an infinite time, but a finite
time. This time should be long compared to the time it takes stars to
go around the galaxy, while still short compared to the time it takes
for them to boil off. Then we'll *approximately* get <T> = -<V>/2.

I talk about this a bit more in another webpage, where I use the virial theorem to study the thermodynamics of gravitating systems. By the way, both that webpage and this one are heavily indebted to discussions with people on sci.physics.research, especially Ted Bunn and Jim Means. I even borrowed some of Ted's exact words in the above discussion about applications to astronomy! He's an astrophysicist; I'm not.

© 2000 John Baez

baez@math.removethis.ucr.andthis.edu