Use units , consistent with comparing directly to , and metric signature . For an arbitrary worldline parameter , an action for a charged relativistic particle is
The first term has variation in its momentum, and the coupling gives . The Euler-Lagrange equations therefore read
When is proper time, has , giving the covariant Lorentz force
With and , put , , for nonzero charge. The velocity equations become
Thus , with , . Integrating with , gives , and . Integrate once more from the origin:
For zero charge the trajectory is simply rest, , with all spatial coordinates zero. The charged trajectory oscillates in while drifting in the negative direction, the direction of . Its displacement-to-time ratio over a proper-time period is . A boost at that drift velocity removes the electric field and leaves circular magnetic motion; in the original frame the orbit has repeating cycloidal cusps where the particle is momentarily at rest. Energy oscillates rather than growing indefinitely because . In SI units the corresponding magnetic-dominated condition is .
For the relativistic particle action , varying the worldline einbein gives . On the positive-einbein branch the proper time satisfies . A reparametrization with sets the transformed einbein to one, making the geodesic equation affinely parametrized. This gauge choice is made after retaining the einbein mass shell constraint; fixing the action first would discard that equation. If the parameter interval is held fixed at both ends, its integrated proper length is a modulus and cannot be arbitrarily changed by endpoint-preserving transformations.