Expansion tensor on rotating disk

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Discussion Overview

The discussion revolves around the calculation of the expansion tensor for a rotating disk in flat spacetime using cylindrical coordinates. Participants explore the necessary steps to define a congruence representing the material of the disk and the implications of its non-constant angular velocity.

Discussion Character

  • Technical explanation
  • Mathematical reasoning
  • Exploratory

Main Points Raised

  • One participant presents the metric for flat spacetime in cylindrical coordinates and introduces the concept of a congruence for the disk's material.
  • Another participant references a Wikipedia article that defines the expansion tensor and suggests that the expansion scalar, calculated as the covariant divergence of the 4-velocity, may be easier to compute than the full expansion tensor.
  • A third participant mentions a paper that provides definitions for the expansion and rotation tensors, noting that the shear tensor vanishes due to the rotational symmetry of the problem.
  • This participant also highlights that the expansion tensor is non-vanishing because the 4-velocity field is not parallel to a time-like Killing field, indicating non-Born rigidity due to non-vanishing vorticity.

Areas of Agreement / Disagreement

Participants generally agree on the vanishing of the shear tensor and the non-vanishing nature of the expansion tensor, but the discussion remains open regarding the specific calculations and implications of these properties.

Contextual Notes

Participants express uncertainty about the detailed calculations required to derive the expansion tensor and its components, indicating a reliance on definitions and existing literature without resolving the mathematical steps involved.

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Hi Everyone,

Suppose that we have cylindrical coordinates on flat spacetime (in units where c=1): ##ds^2 = -dt^2 + dr^2 + r^2 d\theta^2 + dz^2##

I would like to explicitly calculate the expansion tensor for a disk of constant radius R<1 and non-constant angular velocity ##\omega(t)<1##. I don't know how to do this. All I know that it starts with defining a congruence that represents the material of the disk.

Each point on the disk would have a four-velocity of
$$v=\left( \frac{1}{\sqrt{1-r^2 \omega^2}},0, \frac{r\omega}{\sqrt{1-r^2 \omega^2}},0\right) = \gamma \partial_t + r\omega\gamma\partial_{\theta}$$ where ##\gamma=(1-r^2 \omega^2)^{-1/2}##

I think that is the congruence, but where do I go from there?
 
Last edited:
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Wikipedia has a brief definition of the expansion tensor (as well as the other elements of the kinematic decomposition):

http://en.wikipedia.org/wiki/Congru...atical_decomposition_of_a_timelike_congruence

The computations are tedious (at least, I find them so :wink:) but straightforward.

For this particular case, it looks to me like there should be zero shear, so all the information about expansion (if any) should be in the expansion scalar, which is easier to calculate; it's just ##\nabla_a u^a##, i.e., the (covariant) divergence of the 4-velocity.
 
Hi Dale, see http://arxiv.org/pdf/gr-qc/0312087v2.pdf

The authors do not explicitly write out the details of the calculations, rather they simply explicitly write down the expansion and rotation tensors from the definitions, but this does let you check the result of your own calculations.

As Peter remarked, the shear tensor vanishes identically as we would expect given the rotational symmetry of the entire problem. The expansion tensor is non-vanishing of course due to the fact that the 4-velocity field of the time-like congruence is not parallel to a time-like Killing field of flat space-time, which by the Herglotz-Noether theorem implies the non-Born rigidity of the congruence since the 4-velocity field has non-vanishing vorticity.
 
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Thanks Peter and WBN, I will get back to you if I get stuck.
 

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