Kretschmann scalar

In the theory of Lorentzian manifolds, particularly in the context of applications to general relativity, the Kretschmann scalar is a quadratic scalar invariant. It was introduced by Erich Kretschmann.^[1]

Definition

The Kretschmann invariant is^[1][2]

$K = R_{abcd} \, R^{abcd}$

where $R_{abcd}$ is the Riemann curvature tensor. Because it is a sum of squares of tensor components, this is a quadratic invariant.

For a Schwarzschild black hole, the Kretschmann scalar is^[1]

$K = \frac{48 G^2 M^2}{c^4 r^6} \,.$

Relation to other invariants

Another possible invariant (which has been employed for example in writing the gravitational term of the Lagrangian for some higher-order gravity theories) is

$C_{abcd} \, C^{abcd}$

where $C_{{abcd}}$ is the Weyl tensor, the conformal curvature tensor which is also the completely traceless part of the Riemann tensor. In $d$ dimensions this is related to the Kretschmann invariant by^[3]

$R_{abcd} \, R^{abcd} = C_{abcd} \, C^{abcd} +\frac{4}{d-2} R_{ab}\, R^{ab} - \frac{2}{(d-1)(d-2)}R^2$

where $R^{ab}$ is the Ricci curvature tensor and $R$ is the Ricci scalar curvature (obtained by taking successive traces of the Riemann tensor). The Ricci tensor vanishes in vacuum spacetimes (such as the Schwarzschild solution mentioned above), and hence there the Riemann tensor and the Weyl tensor coincide, as do their invariants.

The Kretschmann scalar and the Chern-Pontryagin scalar

$R_{abcd} \, {{}^\star \! R}^{abcd}$

where ${{}^\star R}^{abcd}$ is the left dual of the Riemann tensor, are mathematically analogous (to some extent, physically analogous) to the familiar invariants of the electromagnetic field tensor

$F_{ab} \, F^{ab}, \; \; F_{ab} \, {{}^\star \! F}^{ab}$

See also

• Carminati-McLenaghan invariants, for a set of invariants.
• Classification of electromagnetic fields, for more about the invariants of the electromagnetic field tensor.
• Curvature invariant, for curvature invariants in Riemannian and pseudo-Riemannian geometry in general.
• Curvature invariant (general relativity).
• Ricci decomposition, for more about the Riemann and Weyl tensor.

References

1. Richard C. Henry (2000). "Kretschmann Scalar for a Kerr-Newman Black Hole". The Astrophysical Journal. The American Astronomical Society. 535: 350–353. arXiv:astro-ph/9912320v1. Bibcode:2000ApJ...535..350H. doi:10.1086/308819.
2. Grøn & Hervik 2007, p 219
3. Cherubini, Christian; Bini, Donato; Capozziello, Salvatore; Ruffini, Remo (2002). "Second Order Scalar Invariants of the Riemann Tensor: Applications to Black Hole Spacetimes". International Journal of Modern Physics D. 11 (06): 827–841. arXiv:gr-qc/0302095v1. Bibcode:2002IJMPD..11..827C. doi:10.1142/S0218271802002037. ISSN 0218-2718.

Further reading

• Grøn, Øyvind; Hervik, Sigbjørn (2007), Einstein's General Theory of Relativity, New York: Springer, ISBN 978-0-387-69199-2 Cite uses deprecated parameter |coauthors= (help)
• B. F. Schutz (2009), A First Course in General Relativity (Second Edition), Cambridge University Press, ISBN 978-0-521-88705-2
• Misner, Charles W.; Thorne, Kip. S.; Wheeler, John A. (1973), Gravitation, W. H. Freeman, ISBN 0-7167-0344-0