# Time dilation in the Reissner-Nordström metric [closed]

According to Wikipedia, the formula for gravitational time dilation in the vicinity of a charged mass is:

$$\varsigma = \sqrt{|g^{t t}|} = \sqrt{\frac{r^2}{Q^2+(r-2 M) r}}$$

However, if I plug in $$M=$$Earth, $$r=$$Earth, $$Q=0$$, I get an imaginary number. Just in case I've made a silly mistake, this is, I think, the same formula in swift:

let r = 6e6 // meters
let Q = 0.0 // Coulombs
let M = 5.9e24 // kg

func σ(r: Double, Q: Double, M: Double) -> Double {
let r² = r*r
let Q² = Q*Q

let σ = sqrt( r² / (Q² + (r-(2*M))*r) )
// here, r² / (Q² + (r-(2*M))*r) = -5.084745762711864e-19

return σ
}

print( σ(r: r, Q: Q, M: M) ) // prints "-nan"


This is clearly wrong, so what's the error?

• If you are using SI units, you will need to include factors of $c$ and $G$ to get the dimensions of $M$ correct. Otherwise expressions like $r - 2 M$ make no sense. – Clara Diaz Sanchez Dec 20 '19 at 10:18
• I'm voting to close this question as off-topic because it's about debugging code and not physics concepts. – Kyle Kanos Dec 20 '19 at 11:26
• @KyleKanos having seen what Clara and John have written, I believe my error is definitely about the physics concepts. I didn't realise I'd made the elementary mistake of forgetting units, which would've made the absence of c and G in the equation clear. – BenRW Dec 20 '19 at 13:25

In general relativity we often work with geometrical units in which $$c = G = 1$$ as this greatly simplifies the equations, and this is the form of the equation you are using. To calculate the time dilation you need to put back in the factors of $$c$$ and $$G$$.

The Reissner-Nordstrom metric is:

$$c^2d\tau^2=c^2\left(1-\frac{r_s}{r}+\frac{r_q^2}{r^2}\right)dt^2 - \left(1-\frac{r_s}{r}+\frac{r_q^2}{r^2}\right)^{-1}dr^2 - r^2d\Omega^2$$

where:

$$r_s = \frac{2GM}{c^2}$$

and:

$$r_q^2 = \frac{Q^2G}{4 \pi \epsilon_0 c^4}$$

In this equation $$\tau$$ is the time measured by the observer near the black hole and $$t$$ is the time measured by the observer far from the black hole, so the time dilation factor is $$t/\tau$$. For stationary observers $$dr = d\Omega = 0$$ so the equation simplifies to:

$$\frac{dt}{d\tau} = \left(1-\frac{r_s}{r}+\frac{r_q^2}{r^2}\right)^{-1/2} = \left(1-\frac{2GM}{c^2r}+\frac{GQ^2}{4\pi\epsilon_0c^4r^2}\right)^{-1/2}$$

And this is the equation you need.

• Well, that was an embarrassing thing for me to forget. Thank you for the helpful explanation. – BenRW Dec 20 '19 at 13:29