Ricci scalars (Newman–Penrose formalism)

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In the Newman–Penrose (NP) formalism of general relativity, independent components of the Ricci tensors of a four-dimensional spacetime are encoded into seven (or ten) Ricci scalars which consist of three real scalars \{\Phi_{00}, \Phi_{11}, \Phi_{22}\}, three (or six) complex scalars \{\Phi_{01}=\overline{\Phi_{10}}\,,\Phi_{02}=\overline{\Phi_{20}}\,,\Phi_{12}=\overline{\Phi_{21}}\} and the NP curvature scalar \Lambda. Physically, Ricci-NP scalars are related with the energy–momentum distribution of the spacetime due to Einstein's field equation.

Definitions[edit]

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 Ricci-NP scalars are defined by[1][2][3] (where overline means complex conjugate)

\Phi_{00}:=\frac{1}{2}R_{ab}l^a l^b\,, \quad \Phi_{11}:=\frac{1}{4}R_{ab}(\,l^a n^b+m^a\bar{m}^b)\,, \quad\Phi_{22}:=\frac{1}{2}R_{ab}n^a n^b\,, \quad\Lambda:=\frac{R}{24}\,;

\Phi_{01}:=\frac{1}{2}R_{ab}l^a m^b\,, \quad\; \Phi_{10}:=\frac{1}{2}R_{ab}l^a \bar{m}^b=\overline{\Phi_{01}}\,,
\Phi_{02}:=\frac{1}{2}R_{ab}m^a m^b\,, \quad \Phi_{20}:=\frac{1}{2}R_{ab}\bar{m}^a \bar{m}^b=\overline{\Phi_{02}}\,,
\Phi_{12}:=\frac{1}{2}R_{ab}\bar{m}^a n^b\,, \quad\; \Phi_{21}:=\frac{1}{2}R_{ab}m^a n^b=\overline{\Phi_{12}}\,.

Remark I: In these definitions, R_{ab} could be replaced by its trace-free part  Q_{ab}=R_{ab}-\frac{1}{4}g_{ab}R[2] or by the Einstein tensor  G_{ab}=R_{ab}-\frac{1}{2}g_{ab}R because of the normalization (i.e. inner product) relations that

l_a l^a = n_a n^a = m_a m^a = \bar{m}_a \bar{m}^a=0\,,
l_a m^a = l_a \bar{m}^a = n_a m^a = n_a \bar{m}^a=0\,.

Remark II: Specifically for electrovacuum, we have \Lambda=0, thus

24\Lambda\,=0=\,R_{ab}g^{ab}\,=\,R_{ab}\Big(-2l^a n^b+2m^a\bar{m}^b \Big)\; \Rightarrow \; R_{ab}l^a n^b\,=\,R_{ab}m^a\bar{m}^b\,,

and therefore \Phi_{11} is reduced to

\Phi_{11}:=\frac{1}{4}R_{ab}(\,l^a n^b+m^a\bar{m}^b)=\frac{1}{2}R_{ab}l^a n^b=\frac{1}{2}R_{ab}m^a\bar{m}^a\,.

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

Alternative derivations[edit]

According to the definitions above, one should find out the Ricci tensors before calculating the Ricci-NP scalars via contractions with the corresponding tetrad vectors. However, this method fails to fully reflect the spirit of Newman–Penrose formalism and alternatively, one could compute the spin coefficients and then derive the Ricci-NP scalars \Phi_{ij} via relevant NP field equations that[2][7]

\Phi_{00}=D\rho -\bar{\delta}\kappa-(\rho^2+\sigma\bar{\sigma})-(\varepsilon+\bar{\varepsilon})\rho+\bar{\kappa}\tau+\kappa(3\alpha+\bar{\beta}-\pi)\,,
\Phi_{10}=D\alpha-\bar{\delta}\varepsilon-(\rho+\bar{\varepsilon}-2\varepsilon)\alpha-\beta\bar{\sigma}+\bar{\beta}\varepsilon+\kappa\lambda+\bar{\kappa}\gamma-(\varepsilon+\rho)\pi\,,
\Phi_{02}=\delta\tau-\Delta\sigma-(\mu\sigma+\bar{\lambda}\rho)-(\tau+\beta-\bar{\alpha})\tau+(3\gamma-\bar{\gamma})\sigma+\kappa\bar{\nu}\,,
\Phi_{20}=D\lambda-\bar{\delta}\pi-(\rho\lambda+\bar{\sigma}\mu)-\pi^2-(\alpha-\bar{\beta})\pi+\nu\bar{\kappa}+(3\varepsilon-\bar{\varepsilon})\lambda\,,
\Phi_{12}=\delta\gamma-\Delta\beta-(\tau-\bar{\alpha}-\beta)\gamma-\mu\tau+\sigma\nu+\varepsilon\bar{\nu}+(\gamma-\bar{\gamma}-\mu)\beta-\alpha\bar{\lambda}\,,
\Phi_{22}=\delta\nu-\Delta\mu-(\mu^2+\lambda\bar{\lambda})-(\gamma+\bar{\gamma})\mu+\bar{\nu}\pi-(\tau-3\beta-\bar{\alpha})\nu\,,
2\Phi_{11}=D\gamma-\Delta\varepsilon+\delta\alpha-\bar{\delta}\beta-(\tau+\bar{\pi})\alpha-\alpha\bar{\alpha}-(\bar{\tau}+\pi)\beta-\beta\bar{\beta}+2\alpha\beta+(\varepsilon+\bar{\varepsilon})\gamma-(\rho-\bar{\rho})\gamma+(\gamma+\bar{\gamma})\varepsilon-(\mu-\bar{\mu})\varepsilon-\tau\pi+\nu\kappa-(\mu\rho-\lambda\sigma)\,,

while the NP curvature scalar \Lambda could be directly and easily calculated via \Lambda=\frac{R}{24} with R being the ordinary scalar curvature of the spacetime metric g_{ab}=-l_a  n_b - n_a  l_b +m_a  \bar{m}_b +\bar{m}_a  m_b.

Electromagnetic Ricci-NP scalars[edit]

According to the definitions of Ricci-NP scalars \Phi_{ij} above and the fact that R_{ab} could be replaced by G_{ab} in the definitions, \Phi_{ij} are related with the energy–momentum distribution due to Einstein's field equations G_{ab}=8\pi T_{ab}. In the simplest situation, i.e. vacuum spacetime in the absence of matter fields with T_{ab}=0, we will have \Phi_{ij}=0. Moreover, for electromagnetic field, in addition to the aforementioned definitions, \Phi_{ij} could be determined more specifically by[1]


\Phi_{ij}=\,2\,\phi_i\,\overline{\phi_j}\,,\quad (i,j\in\{0,1,2\})\,,

where \phi_i denote the three complex Maxwell-NP scalars[1] which encode the six independent components of the Faraday-Maxwell 2-form F_{ab} (i.e. the electromagnetic field strength tensor)


\phi_0:= -F_{ab}l^a m^b \,,\quad \phi_1:= -\frac{1}{2} F_{ab}\big(l^an^a-m^a\bar{m}^b \big)\,, \quad \phi_2 := F_{ab} n^a \bar{m}^b\,.

Remark: The equation \Phi_{ij}=2\,\phi_i\, \overline{\phi_j} for electromagnetic field is however not necessarily valid for other kinds of matter fields. For example, in the case of Yang–Mills fields there will be \Phi_{ij}=\,\text{Tr}\,(\digamma_i \,\bar{\digamma}_j) where \digamma_i (i\in\{0,1,2 \}) are Yang–Mills-NP scalars.[8]

See also[edit]

References[edit]

  1. ^ a b c Jeremy Bransom Griffiths, Jiri Podolsky. Exact Space-Times in Einstein's General Relativity. Cambridge: Cambridge University Press, 2009. Chapter 2.
  2. ^ a b c 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. ^ a b Peter O'Donnell. Introduction to 2-Spinors in General Relativity. Singapore: World Scientific, 2003.
  8. ^ E T Newman, K P Tod. Asymptotically Flat Spacetimes, Appendix A.2. In A Held (Editor): General Relativity and Gravitation: One Hundred Years After the Birth of Albert Einstein. Vol (2), page 27. New York and London: Plenum Press, 1980.