Reissner–Nordström metric

In spherical coordinates ${\displaystyle (t,r,\theta ,\varphi )}$, the Reissner–Nordström metric (i.e. the line element) is ${\displaystyle ds^{2}=c^{2}\,d\tau ^{2}=\left(1-{\frac {r_{\text{s}}}{r}}+{\frac {r_{\rm {Q}}^{2}}{r^{2}}}\right)c^{2}\,dt^{2}-\left(1-{\frac {r_{\text{s}}}{r}}+{\frac {r_{Q}^{2}}{r^{2}}}\right)^{-1}\,dr^{2}-r^{2}\,d\theta ^{2}-r^{2}\sin ^{2}\theta \,d\varphi ^{2},}$ where ${\displaystyle c}$ is the speed of light, ${\displaystyle \tau }$ is the proper time, ${\displaystyle t}$ is the time coordinate (measured by a stationary clock at infinity), ${\displaystyle r}$ is the radial coordinate, ${\displaystyle (\theta ,\varphi )}$ are the spherical angles, and ${\displaystyle r_{\text{s}}}$ is the Schwarzschild radius of the body given by ${\displaystyle r_{\text{s}}={\frac {2GM}{c^{2}}},}$ and ${\displaystyle r_{Q}}$ is a characteristic length scale given by ${\displaystyle r_{Q}^{2}={\frac {Q^{2}G}{4\pi \varepsilon _{0}c^{4}}}.}$ Here, ${\displaystyle \varepsilon _{0}}$ is the electric constant.

The total mass of the central body and its irreducible mass are related by[6][7] ${\displaystyle M_{\rm {irr}}={\frac {c^{2}}{G}}{\sqrt {\frac {r_{+}^{2}}{2}}}\ \to \ M={\frac {Q^{2}}{16\pi \varepsilon _{0}GM_{\rm {irr}}}}+M_{\rm {irr}}.}$

The difference between ${\displaystyle M}$ and ${\displaystyle M_{\rm {irr}}}$ is due to the equivalence of mass and energy, which makes the electric field energy also contribute to the total mass.

In the limit that the charge ${\displaystyle Q}$ (or equivalently, the length scale ${\displaystyle r_{Q}}$) goes to zero, one recovers the Schwarzschild metric. The classical Newtonian theory of gravity may then be recovered in the limit as the ratio ${\displaystyle r_{\text{s}}/r}$ goes to zero. In the limit that both ${\displaystyle r_{Q}/r}$ and ${\displaystyle r_{\text{s}}/r}$ go to zero, the metric becomes the Minkowski metric for special relativity.

In practice, the ratio ${\displaystyle r_{\text{s}}/r}$ is often extremely small. For example, the Schwarzschild radius of the Earth is roughly 9 mm (3/8 inch), whereas a satellite in a geosynchronous orbit has an orbital radius ${\displaystyle r}$ that is roughly four billion times larger, at 42,164 km (26,200 miles). Even at the surface of the Earth, the corrections to Newtonian gravity are only one part in a billion. The ratio only becomes large close to black holes and other ultra-dense objects such as neutron stars.

Although charged black holes with r_Q ≪ r_s are similar to the Schwarzschild black hole, they have two horizons: the event horizon and an internal Cauchy horizon.[8] As with the Schwarzschild metric, the event horizons for the spacetime are located where the metric component ${\displaystyle g_{rr}}$ diverges; that is, where

$${\displaystyle 1-{\frac {r_{\rm {s}}}{r}}+{\frac {r_{\rm {Q}}^{2}}{r^{2}}}=-{\frac {1}{g_{rr}}}=0.}$$

This equation has two solutions:

$${\displaystyle r_{\pm }={\frac {1}{2}}\left(r_{\rm {s}}\pm {\sqrt {r_{\rm {s}}^{2}-4r_{\rm {Q}}^{2}}}\right).}$$

These concentric event horizons become degenerate for 2r_Q = r_s, which corresponds to an extremal black hole. Black holes with 2r_Q > r_s cannot exist in nature because if the charge is greater than the mass there can be no physical event horizon (the term under the square root becomes negative).[9] Objects with a charge greater than their mass can exist in nature, but they can not collapse down to a black hole, and if they could, they would display a naked singularity.[10] Theories with supersymmetry usually guarantee that such "superextremal" black holes cannot exist.

The electromagnetic potential is

$${\displaystyle A_{\alpha }=(Q/r,0,0,0).}$$

If magnetic monopoles are included in the theory, then a generalization to include magnetic charge P is obtained by replacing Q² by Q² + P² in the metric and including the term P cos θ dφ in the electromagnetic potential.

The gravitational time dilation in the vicinity of the central body is given by

$${\displaystyle \gamma ={\sqrt {|g^{tt}|}}={\sqrt {\frac {r^{2}}{Q^{2}+(r-2M)r}}},}$$

which relates to the local radial escape velocity of a neutral particle

$${\displaystyle v_{\rm {esc}}={\frac {\sqrt {\gamma ^{2}-1}}{\gamma }}.}$$

The Christoffel symbols

$${\displaystyle \Gamma _{jk}^{i}=\sum _{s=0}^{3}\ {\frac {g^{is}}{2}}\left({\frac {\partial g_{js}}{\partial x^{k}}}+{\frac {\partial g_{sk}}{\partial x^{j}}}-{\frac {\partial g_{jk}}{\partial x^{s}}}\right)}$$

with the indices

$${\displaystyle \{0,\ 1,\ 2,\ 3\}\to \{t,\ r,\ \theta ,\ \varphi \}}$$

give the nonvanishing expressions

$${\displaystyle {\begin{aligned}\Gamma _{tr}^{t}&={\frac {Mr-Q^{2}}{r(Q^{2}+r^{2}-2Mr)}}\\[6pt]\Gamma _{tt}^{r}&={\frac {(Mr-Q^{2})\left(r^{2}-2Mr+Q^{2}\right)}{r^{5}}}\\[6pt]\Gamma _{rr}^{r}&=-{\frac {Q^{2}-Mr}{r(Q^{2}-2Mr+r^{2})}}\\[6pt]\Gamma _{\theta \theta }^{r}&=-{\frac {r^{2}-2Mr+Q^{2}}{r}}\\[6pt]\Gamma _{\varphi \varphi }^{r}&=-{\frac {\sin ^{2}\theta \left(r^{2}-2Mr+Q^{2}\right)}{r}}\\[6pt]\Gamma _{\theta r}^{\theta }&={\frac {1}{r}}\\[6pt]\Gamma _{\varphi \varphi }^{\theta }&=-\sin \theta \cos \theta \\[6pt]\Gamma _{\varphi r}^{\varphi }&={\frac {1}{r}}\\[6pt]\Gamma _{\varphi \theta }^{\varphi }&=\cot \theta \end{aligned}}}$$

Given the Christoffel symbols, one can compute the geodesics of a test-particle.[11][12]

Instead of working in the holonomic basis, one can perform efficient calculations with a tetrad.[13] Let ${\displaystyle {\bf {e}}_{I}=e_{\mu I}}$ be a set of one-forms with internal Minkowski index ${\displaystyle I\in \{0,1,2,3\}}$, such that ${\displaystyle \eta ^{IJ}e_{\mu I}e_{\nu J}=g_{\mu \nu }}$. The Reissner metric can be described by the tetrad

${\displaystyle {\bf {e}}_{0}=G^{1/2}\,dt}$,

${\displaystyle {\bf {e}}_{1}=G^{-1/2}\,dr}$,

${\displaystyle {\bf {e}}_{2}=r\,d\theta }$

${\displaystyle {\bf {e}}_{3}=r\sin \theta \,d\varphi }$

where ${\displaystyle G(r)=1-r_{s}r^{-1}+r_{Q}^{2}r^{-2}}$. The parallel transport of the tetrad is captured by the connection one-forms ${\displaystyle {\boldsymbol {\omega }}_{IJ}=-{\boldsymbol {\omega }}_{JI}=\omega _{\mu IJ}=e_{I}^{\nu }\nabla _{\mu }e_{J\nu }}$. These have only 24 independent components compared to the 40 components of ${\displaystyle \Gamma _{\mu \nu }^{\lambda }}$. The connections can be solved for by inspection from Cartan's equation ${\displaystyle d{\bf {e}}_{I}={\bf {e}}^{J}\wedge {\boldsymbol {\omega }}_{IJ}}$, where the left hand side is the exterior derivative of the tetrad, and the right hand side is a wedge product.

${\displaystyle {\boldsymbol {\omega }}_{10}={\frac {1}{2}}\partial _{r}G\,dt}$

${\displaystyle {\boldsymbol {\omega }}_{20}={\boldsymbol {\omega }}_{30}=0}$

${\displaystyle {\boldsymbol {\omega }}_{21}=-G^{1/2}\,d\theta }$

${\displaystyle {\boldsymbol {\omega }}_{31}=-\sin \theta G^{1/2}d\varphi }$

${\displaystyle {\boldsymbol {\omega }}_{32}=-\cos \theta \,d\varphi }$

The Riemann tensor ${\displaystyle {\bf {R}}_{IJ}=R_{\mu \nu IJ}}$ can be constructed as a collection of two-forms by the second Cartan equation ${\displaystyle {\bf {R}}_{IJ}=d{\boldsymbol {\omega }}_{IJ}+{\boldsymbol {\omega }}_{IK}\wedge {\boldsymbol {\omega }}^{K}{}_{J},}$ which again makes use of the exterior derivative and wedge product. This approach is significantly faster than the traditional computation with ${\displaystyle \Gamma _{\mu \nu }^{\lambda }}$; note that there are only four nonzero ${\displaystyle {\boldsymbol {\omega }}_{IJ}}$ compared with nine nonzero components of ${\displaystyle \Gamma _{\mu \nu }^{\lambda }}$.

[14]

Because of the spherical symmetry of the metric, the coordinate system can always be aligned in a way that the motion of a test-particle is confined to a plane, so for brevity and without restriction of generality we use θ instead of φ. In dimensionless natural units of G = M = c = K = 1 the motion of an electrically charged particle with the charge q is given by

$${\displaystyle {\ddot {x}}^{i}=-\sum _{j=0}^{3}\ \sum _{k=0}^{3}\ \Gamma _{jk}^{i}\ {{\dot {x}}^{j}}\ {{\dot {x}}^{k}}+q\ {F^{ik}}\ {{\dot {x}}_{k}}}$$

which yields

$${\displaystyle {\ddot {t}}={\frac {\ 2(Q^{2}-Mr)}{r(r^{2}-2Mr+Q^{2})}}{\dot {r}}{\dot {t}}+{\frac {qQ}{(r^{2}-2mr+Q^{2})}}\ {\dot {r}}}$$

$${\displaystyle {\ddot {r}}={\frac {(r^{2}-2Mr+Q^{2})(Q^{2}-Mr)\ {\dot {t}}^{2}}{r^{5}}}+{\frac {(Mr-Q^{2}){\dot {r}}^{2}}{r(r^{2}-2Mr+Q^{2})}}+{\frac {(r^{2}-2Mr+Q^{2})\ {\dot {\theta }}^{2}}{r}}+{\frac {qQ(r^{2}-2mr+Q^{2})}{r^{4}}}\ {\dot {t}}}$$

$${\displaystyle {\ddot {\theta }}=-{\frac {2\ {\dot {\theta }}\ {\dot {r}}}{r}}.}$$

All total derivatives are with respect to proper time ${\displaystyle {\dot {a}}={\frac {da}{d\tau }}}$.

Constants of the motion are provided by solutions ${\displaystyle S(t,{\dot {t}},r,{\dot {r}},\theta ,{\dot {\theta }},\varphi ,{\dot {\varphi }})}$ to the partial differential equation[15]

$${\displaystyle 0={\dot {t}}{\dfrac {\partial S}{\partial t}}+{\dot {r}}{\frac {\partial S}{\partial r}}+{\dot {\theta }}{\frac {\partial S}{\partial \theta }}+{\ddot {t}}{\frac {\partial S}{\partial {\dot {t}}}}+{\ddot {r}}{\frac {\partial S}{\partial {\dot {r}}}}+{\ddot {\theta }}{\frac {\partial S}{\partial {\dot {\theta }}}}}$$

after substitution of the second derivatives given above. The metric itself is a solution when written as a differential equation

$${\displaystyle S_{1}=1=\left(1-{\frac {r_{s}}{r}}+{\frac {r_{\rm {Q}}^{2}}{r^{2}}}\right)c^{2}\,{\dot {t}}^{2}-\left(1-{\frac {r_{s}}{r}}+{\frac {r_{Q}^{2}}{r^{2}}}\right)^{-1}\,{\dot {r}}^{2}-r^{2}\,{\dot {\theta }}^{2}.}$$

The separable equation

$${\displaystyle {\frac {\partial S}{\partial r}}-{\frac {2}{r}}{\dot {\theta }}{\frac {\partial S}{\partial {\dot {\theta }}}}=0}$$

immediately yields the constant relativistic specific angular momentum

$${\displaystyle S_{2}=L=r^{2}{\dot {\theta }};}$$

a third constant obtained from

$${\displaystyle {\frac {\partial S}{\partial r}}-{\frac {2(Mr-Q^{2})}{r(r^{2}-2Mr+Q^{2})}}{\dot {t}}{\frac {\partial S}{\partial {\dot {t}}}}=0}$$

is the specific energy (energy per unit rest mass)[16]

$${\displaystyle S_{3}=E={\frac {{\dot {t}}(r^{2}-2Mr+Q^{2})}{r^{2}}}+{\frac {qQ}{r}}.}$$

Substituting ${\displaystyle S_{2}}$ and ${\displaystyle S_{3}}$ into ${\displaystyle S_{1}}$ yields the radial equation

$${\displaystyle c\int d\,\tau =\int {\frac {r^{2}\,dr}{\sqrt {r^{4}(E-1)+2Mr^{3}-(Q^{2}+L^{2})r^{2}+2ML^{2}r-Q^{2}L^{2}}}}.}$$

Multiplying under the integral sign by ${\displaystyle S_{2}}$ yields the orbital equation

$${\displaystyle c\int Lr^{2}\,d\theta =\int {\frac {L\,dr}{\sqrt {r^{4}(E-1)+2Mr^{3}-(Q^{2}+L^{2})r^{2}+2ML^{2}r-Q^{2}L^{2}}}}.}$$

The total time dilation between the test-particle and an observer at infinity is

$${\displaystyle \gamma ={\frac {q\ Q\ r^{3}+E\ r^{4}}{r^{2}\ (r^{2}-2r+Q^{2})}}.}$$

The first derivatives ${\displaystyle {\dot {x}}^{i}}$ and the contravariant components of the local 3-velocity ${\displaystyle v^{i}}$ are related by

$${\displaystyle {\dot {x}}^{i}={\frac {v^{i}}{\sqrt {(1-v^{2})\ |g_{ii}|}}},}$$

which gives the initial conditions

$${\displaystyle {\dot {r}}={\frac {v_{\parallel }{\sqrt {r^{2}-2M+Q^{2}}}}{r{\sqrt {(1-v^{2})}}}}}$$

$${\displaystyle {\dot {\theta }}={\frac {v_{\perp }}{r{\sqrt {(1-v^{2})}}}}.}$$

The specific orbital energy

$${\displaystyle E={\frac {\sqrt {Q^{2}-2rM+r^{2}}}{r{\sqrt {1-v^{2}}}}}+{\frac {qQ}{r}}}$$

and the specific relative angular momentum

$${\displaystyle L={\frac {v_{\perp }\ r}{\sqrt {1-v^{2}}}}}$$

of the test-particle are conserved quantities of motion. ${\displaystyle v_{\parallel }}$ and ${\displaystyle v_{\perp }}$ are the radial and transverse components of the local velocity-vector. The local velocity is therefore

$${\displaystyle v={\sqrt {v_{\perp }^{2}+v_{\parallel }^{2}}}={\sqrt {\frac {(E^{2}-1)r^{2}-Q^{2}-r^{2}+2rM}{E^{2}r^{2}}}}.}$$

The metric can be expressed in Kerr–Schild form like this:

$${\displaystyle {\begin{aligned}g_{\mu \nu }&=\eta _{\mu \nu }+fk_{\mu }k_{\nu }\\[5pt]f&={\frac {G}{r^{2}}}\left[2Mr-Q^{2}\right]\\[5pt]\mathbf {k} &=(k_{x},k_{y},k_{z})=\left({\frac {x}{r}},{\frac {y}{r}},{\frac {z}{r}}\right)\\[5pt]k_{0}&=1.\end{aligned}}}$$

Notice that k is a unit vector. Here M is the constant mass of the object, Q is the constant charge of the object, and η is the Minkowski tensor.

In certain approaches to quantum gravity, the classical Reissner–Nordström metric receives quantum corrections. An example of this is given by the effective field theory approach pioneered by Barvinsky and Vilkovisky.[17][18][19][20] At second order in curvature, the classical Einstein-Hilbert action is supplemented by local and non-local terms:

${\displaystyle \Gamma =\int d^{4}x\,{\sqrt {-g}}\,{\bigg (}{\frac {R}{16\pi G_{N}}}+c_{1}(\mu )R^{2}+c_{2}(\mu )R_{\mu \nu }R^{\mu \nu }+c_{3}(\mu )R_{\mu \nu \rho \sigma }R^{\mu \nu \rho \sigma }{\bigg )}-\int d^{4}x{\sqrt {-g}}{\bigg [}\alpha R\ln \left({\frac {\Box }{\mu ^{2}}}\right)R+\beta R_{\mu \nu }\ln \left({\frac {\Box }{\mu ^{2}}}\right)R^{\mu \nu }+\gamma R_{\mu \nu \rho \sigma }\ln \left({\frac {\Box }{\mu ^{2}}}\right)R^{\mu \nu \rho \sigma }{\bigg ]},}$

where ${\displaystyle \mu }$ is an energy scale. The exact values of the coefficients ${\displaystyle c_{1},c_{2},c_{3}}$ are unknown, as they depend on the nature of the ultra-violet theory of quantum gravity. On the other hand, the coefficients ${\displaystyle \alpha ,\beta ,\gamma }$ are calculable.[21] The operator ${\displaystyle \ln \left(\Box /\mu ^{2}\right)}$ has the integral representation

${\displaystyle \ln \left({\frac {\Box }{\mu ^{2}}}\right)=\int _{0}^{+\infty }ds\,\left({\frac {1}{\mu ^{2}+s}}-{\frac {1}{\Box +s}}\right).}$

The new additional terms in the action imply a modification of the classical solution. The quantum corrected Reissner–Nordström metric, up to order ${\displaystyle {\mathcal {O}}(G^{2})}$, was found by Campos Delgado:[22]

${\displaystyle ds^{2}=-f(r)dt^{2}+{\frac {1}{g(r)}}dr^{2}+r^{2}d\theta ^{2}+r^{2}\sin ^{2}\theta d\phi ^{2},}$

where

${\displaystyle f(r)=1-{\frac {2GM}{r}}+{\frac {GQ^{2}}{r^{2}}}-{\frac {32\pi G^{2}Q^{2}}{r^{4}}}{\bigg [}c_{2}+4c_{3}+2\left(\beta +4\gamma \right)\left(\ln \left(\mu r\right)+\gamma _{E}-{\frac {3}{2}}\right){\bigg ]},}$

${\displaystyle g(r)=1-{\frac {2GM}{r}}+{\frac {GQ^{2}}{r^{2}}}-{\frac {64\pi G^{2}Q^{2}}{r^{4}}}{\Big [}c_{2}+4c_{3}+2\left(\beta +4\gamma \right)\left(\ln \left(\mu r\right)+\gamma _{E}-2\right){\Big ]}.}$

• Black hole electron

• Adler, R.; Bazin, M.; Schiffer, M. (1965). Introduction to General Relativity. New York: McGraw-Hill Book Company. pp. 395–401. ISBN 978-0-07-000420-7.
• Wald, Robert M. (1984). General Relativity. Chicago: The University of Chicago Press. pp. 158, 312–324. ISBN 978-0-226-87032-8. Retrieved 27 April 2013.

• spacetime diagrams including Finkelstein diagram and Penrose diagram, by Andrew J. S. Hamilton
• "Particle Moving Around Two Extreme Black Holes" by Enrique Zeleny, The Wolfram Demonstrations Project.