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Weyl scalar

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 Title: Weyl scalar Author: World Heritage Encyclopedia Language: English Subject: Collection: General Relativity Publisher: World Heritage Encyclopedia Publication Date:

Weyl scalar

In the Newman–Penrose (NP) formalism of general relativity, Weyl scalars refer to a set of five complex scalars \{\Psi_0, \Psi_1, \Psi_2,\Psi_3, \Psi_4\} which encode the ten independent components of the Weyl tensors of a four-dimensional spacetime.

Contents

• Definitions 1
• Alternative derivations 2
• Physical interpretation 3
• References 5

Definitions

Given a complex null tetrad \{l^a, n^a, m^a, \bar{m}^a\} and with the convention \{(-,+,+,+); l^a n_a=-1\,,m^a \bar{m}_a=1\}, the Weyl-NP scalars are defined by[1][2][3]

\Psi_0 := C_{\alpha\beta\gamma\delta} l^\alpha m^\beta l^\gamma m^\delta\ ,
\Psi_1 := C_{\alpha\beta\gamma\delta} l^\alpha n^\beta l^\gamma m^\delta\ ,
\Psi_2 := C_{\alpha\beta\gamma\delta} l^\alpha m^\beta \bar{m}^\gamma n^\delta\ ,
\Psi_3 := C_{\alpha\beta\gamma\delta} l^\alpha n^\beta \bar{m}^\gamma n^\delta\ ,
\Psi_4 := C_{\alpha\beta\gamma\delta} n^\alpha \bar{m}^\beta n^\gamma \bar{m}^\delta\ .

Note: If one adopts the convention \{(+,-,-,-); l^a n_a=1\,,m^a \bar{m}_a=-1\}, the definitions of \Psi_i should take the opposite values;[4][5][6][7] that is to say, \Psi_i\mapsto-\Psi_i after the signature transition.

Alternative derivations

According to the definitions above, one should find out the Weyl tensors before calculating the Weyl-NP scalars via contractions with relevant tetrad vectors. This method, however, does not fully reflect the spirit of Newman–Penrose formalism. As an alternative, one could firstly compute the spin coefficients and then derive the five Weyl-NP scalars via the following NP field equations,

\Psi_0=D\sigma-\delta\kappa-(\rho+\bar{\rho})\sigma-(3\varepsilon-\bar{\varepsilon})\sigma+(\tau-\bar{\pi}+\bar{\alpha}+3\beta)\kappa\,,
\Psi_1=D\beta-\delta\varepsilon-(\alpha+\pi)\sigma-(\bar{\rho}-\bar{\varepsilon})\beta+(\mu+\gamma)\kappa+(\bar{\alpha}-\bar{\pi})\varepsilon\,,
\Psi_2=\bar{\delta}\tau-\Delta\rho-(\rho\bar{\mu}+\sigma\lambda)+(\bar{\beta}-\alpha-\bar{\tau})\tau+(\gamma+\bar{\gamma})\rho+\nu\kappa-2\Lambda\,,
\Psi_3=\bar{\delta}\gamma-\Delta\alpha+(\rho+\varepsilon)\nu-(\tau+\beta)\lambda+(\bar{\gamma}-\bar{\mu})\alpha+(\bar{\beta}-\bar{\tau})\gamma\,.
\Psi_4=\delta\nu-\Delta\lambda-(\mu+\bar{\mu})\lambda-(3\gamma-\bar{\gamma})\lambda+(3\alpha+\bar{\beta}+\pi-\bar{\tau})\nu\,.

where \Lambda (used for \Psi_2) refers to the NP curvature scalar \Lambda:=\frac{R}{24} which could be calculated directly from the spacetime metric g_{ab}.

Physical interpretation

Szekeres (1965)[8] gave an interpretation of the different Weyl scalars at large distances:

\Psi_2 is a "Coulomb" term, representing the gravitational monopole of the source;
\Psi_1 & \Psi_3 are ingoing and outgoing "longitudinal" radiation terms;
\Psi_0 & \Psi_4 are ingoing and outgoing "transverse" radiation terms.

For a general asymptotically flat spacetime containing radiation (Petrov Type I), \Psi_1 & \Psi_3 can be transformed to zero by an appropriate choice of null tetrad. Thus these can be viewed as gauge quantities.

A particularly important case is the Weyl scalar \Psi_4. It can be shown to describe outgoing gravitational radiation (in an asymptotically flat spacetime) as

\Psi_4 = \frac{1}{2}\left( \ddot{h}_{\hat{\theta} \hat{\theta}} - \ddot{h}_{\hat{\phi} \hat{\phi}} \right) + i \ddot{h}_{\hat{\theta}\hat{\phi}} = -\ddot{h}_+ + i \ddot{h}_\times\ .

Here, h_+ and h_\times are the "plus" and "cross" polarizations of gravitational radiation, and the double dots represent double time-differentiation.

There are, however, certain examples in which the interpretation listed above fails.[9] These are exact vacuum solutions of the Einstein field equations with cylindrical symmetry. For instance, a static (infinitely long) cylinder can produce a gravitational field which has not only the expected "Coulomb"-like Weyl component \Psi_2, but also non-vanishing "transverse wave"-components \Psi_0 and \Psi_4. Furthermore, purely outgoing Einstein-Rosen waves have a non-zero "incoming transverse wave"-component \Psi_0.

References

1. ^ Jeremy Bransom Griffiths, Jiri Podolsky. Exact Space-Times in Einstein's General Relativity. Cambridge: Cambridge University Press, 2009. Chapter 2.
2. ^ Valeri P Frolov, Igor D Novikov. Black Hole Physics: Basic Concepts and New Developments. Berlin: Springer, 1998. Appendix E.
3. ^ Abhay Ashtekar, Stephen Fairhurst, Badri Krishnan. Isolated horizons: Hamiltonian evolution and the first law. Physical Review D, 2000, 62(10): 104025. Appendix B. gr-qc/0005083
4. ^ Ezra T Newman, Roger Penrose. An Approach to Gravitational Radiation by a Method of Spin Coefficients. Journal of Mathematical Physics, 1962, 3(3): 566-768.
5. ^ Ezra T Newman, Roger Penrose. Errata: An Approach to Gravitational Radiation by a Method of Spin Coefficients. Journal of Mathematical Physics, 1963, 4(7): 998.
6. ^ Subrahmanyan Chandrasekhar. The Mathematical Theory of Black Holes. Chicago: University of Chikago Press, 1983.
7. ^ Peter O'Donnell. Introduction to 2-Spinors in General Relativity. Singapore: World Scientific, 2003.
8. ^ .
9. ^
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