**Difficulty level:**☆

# Author: colin

## Tetrad for Schwarzschild metric

**Difficulty level:**★ ★ ★ ★

Suppose an observer **u** moves radially with speed (3-velocity) relative to “stationary” Schwarzschild observers, where we define as inward motion. Then one natural choice of orthonormal tetrad is:

where the components are given in Schwarzschild coordinates. This may be derived as follows.

The Schwarzschild observer has 4-velocity

because the spatial coordinates are fixed, and the *t*-component follows from normalisation (Hartle §9.2).

Now the Lorentz factor for the relative speed satisfies , and together with normalisation and the assumption that the θ and φ components are zero, this yields given above.

We obtain by orthonormality: and , and again making the assumption the θ and φ components are zero. Note the negative of the *r*-component is probably an equally natural choice. Then and follow from simply normalising the coordinate vectors.

Strictly speaking this setup only applies for , because stationary timelike observers cannot exist inside a black hole event horizon! Yet remarkably the formulae can work out anyway (MTW …) . An alternate approach is local Lorentz boost described shortly.

Hartle … Also check no “twisting” etc…

## Centenary of General Relativity

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2015 is the 100-year anniversary general relativity. Einstein completed the final version of the field equations in November 1915. As today is the last day of the year, had to get this post in!

## Lorentz factor identity

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A simple but useful identity is:

This follows from the definition of the Lorentz factor γ in terms of a relative speed *V* between two frames:

So

Alternatively raise both sides of the γ defining formula to the power of -2, obtaining , then multiply both sides by γ^{2} and rearrange.

## Radial motion in the Schwarzschild metric, relative to stationary observers

**Difficulty level:**★ ★ ★

Last time we derived the 4-velocity **u** of a small test body moving radially in the Schwarzschild geometry, in terms of *e*, the “energy per unit rest mass”. Another parametrisation is in terms of the 3-speed *V* relative to stationary observers. This turns out to be, in Schwarzschild coordinate expression,

To derive this, first consider the 4-velocity of stationary observers:

We know the “moving” body has 4-velocity **u** of form since the motion is radial. The Lorentz factor for the relative speed is

Evaluating and rearranging yields . Normalisation leads to , after some algebra including use of the identity . We allow also, and define this as inward motion. Carefully considering the sign, this results in the top equation. (An alternate derivation is to perform a local Lorentz boost. *Later articles will discuss this*… The Special Relativity formulae cannot be applied directly to Schwarzschild coordinates.)

Some special cases are noteworthy. For *V*=0, γ=1, and **u** reduces to **u**_{Schw}. This corresponds to . Also we can relate the parametrisation by *V* (and γ) to the parametrisation by *e* via

where the leftmost equation follows from the definition , and subsequently the rightmost equation from γ=γ(*V*). For raindrops with *e*=1, the relative speed reduces to .

We would expect the construction to fail for , as stationary timelike observers cannot exist there, and so the relative speed to them would become meaningless. But curiously, it can actually work for a faster-than-light *V*>1 “Lorentz” boost, as even the authorities MTW (§31.2, explicit acknowledgement) and Taylor & Wheeler (§B.4, implicitly *v*_{rel}>1 for *r*<2*M*) attest. Sometime, I will investigate this further…

## Radial motion in the Schwarzschild metric, in terms of *e*

**Difficulty level:**★ ★ ★

A nice way to parametrise the 4-velocity **u** of a small test body moving radially within Schwarzschild spacetime is by the “energy per unit rest mass” *e*:

For the “±” term, choose the sign based on whether the motion is inwards or outwards. All components are given in Schwarzschild coordinates . The result was derived as follows. In geometric units, the metric is:

By definition , where is the Killing vector corresponding to the independence of the metric from *t*, and has components (Hartle §9.3). For geodesic (freefalling) motion *e* is invariant, however even for accelerated motion *e* is well-defined instantaneously and makes a useful parametrisation.

We want to find say. Rearranging the defining equation for *e* gives . Radial motion means , so the normalised condition yields the remaining component . The resulting formula is valid for all , and for *e*=1 the 4-velocity describes “raindrops” as expected.

## Relative speed

**Difficulty level:**★ ★

Suppose two observers at the same place and time (that is, “event”) move with 4-velocities **u** and **v** respectively, then they measure their relative speed as follows. The Lorentz factor is simply

(The dot is not the Euclidean dot product, but uses the metric: where the indices and are summed over by the Einstein summation convention.) The proof is based on the axiom that some local inertial frame exists, although interestingly one does not need to explicitly construct it.

The relative 3-speed *V*, may then be recovered via:

See for instance Carroll (end of §2.5) who terms it “ordinary three-velocity”. Other sources express the first formula more indirectly, in terms of the energy and momentum measured by an observer : where is the 4-momentum of another observer/object, and combine this with (MTW Exercise 2.5 in §2.8 term it “ordinary velocity”, or Hartle §5.6, and Example 9.1 in §9.3).

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## Welcome!

This is a resource for **general relativity**, which is Einstein’s theory of space, time, and gravity. It includes the related fields of **astrophysics** and **cosmology**, which use physics to study the universe. Later, I will likely stray into **quantum mechanics** and **philosophy of science**.

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I am a university student studying physics, currently in a Master of Science degree. I intend to start a PhD in relativity soon. Join me on the journey, and we’ll see where it leads!