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.
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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