Aichelburg-Sexl ultraboost

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In general relativity, the Aichelburg/Sexl ultraboost is an exact solution which models the physical experience of an observer moves past a spherically symmetric gravitating object at nearly the speed of light. It was introduced by Peter C. Aichelburg and Roman U. Sexl in 1971.

The metric tensor can be written, in terms of Brinkmann coordinates, as

ds^2 = -8m \, \delta(u) \, \log r \, du^2 + 2 \, du \, dv + dr^2 + r^2 \, d\theta^2,
-\infty < u < \infty, \, 0 < r < \infty, \, -\infty < v < \infty, -\pi < \theta < \pi

The ultraboost can be obtained as the limit of various sequences smooth Lorentzian manifolds. For example, we can take Poor-man's Gaussian pulses

ds^2 = -\frac{4 m a \, \log(r)}{\pi \, (1+a^2 u^2)} \, du^2 - 2 du \, dv + dr^2 + r^2 \, d\theta^2,
-\infty < u < \infty, \, 0 < r < \infty, \, -\infty < v < \infty, -\pi < \theta < \pi

In these plus-polarized axisymmetric vacuum pp-waves, the curvature is concentrated along the axis of symmetry, falling off like O(m/r), and also near u = 0. As a \rightarrow \infty, the wave profile turns into a Dirac delta, and we recover the ultraboost. (To avoid possible misunderstanding, we stress that these are exact solutions which approximate the ultraboost, which is also an exact solution, at least if you admit impulsive curvatures.)

[edit] References

  • Frolov, Valeri P.; & Novikov, Igor D. (1998). Black Hole Physics. Boston: Klüwer. ISBN 0-7923-5146-0.  See Section 7.6.12
  • Poldolský, J.; & Griffiths, J. B. (1998). "Boosted static multipole particles as sources of impulsive gravitational waves". Phys. Rev. D 58: 124024.  See also Boosted static multipole particles as sources of impulsive gravitational waves. ArXiv. Retrieved on 15 June, 2005.
  • Aichelburg, P. C.; & Sexl, R. U. (1971). "On the gravitational field of a massless particle". Gen. Rel. Grav. 2: 303. 
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