How find out the expression of Einstein tensor? I am studying the Schwarzschild solution of the Einstein field equation in vacuum and I have encountered a problem in obtaining the expression for Einstein tensor for the following metric $g$ considered, i.e the spherically symmetric metric in Schwarzschild coordinates:
$$g=-e^{2\nu}dt^2+e^{2\lambda}dr^2+r^2d\Omega^2$$ with $d\Omega^2=d\theta^2+\sin{\theta}^2d\phi^2$.
So this is associated to the metric $g_{\alpha \beta}=\begin{pmatrix}
-e^{2\nu} & 0 & 0 & 0\\
0 & e^{2\lambda} & 0 & 0\\
0 & 0 & r^2& 0\\
0 & 0 & 0 & r^2\sin{\theta}^2\\
\end{pmatrix}$
Now in order to write down the Einstein tensor, to solve the Einstein field equation, I have to consider that $G_{\mu\nu}=0\iff G_{\beta}^{\alpha}=g^{\alpha\mu}G_{\mu\beta}=0$ since $g$ is no degenerate.
But now my problem is to determine the components $G_{\beta}^{\alpha}$!
I have read I should obtain:
$$G_0^0=\frac{-1}{r^2}+e^{-2\lambda}(\frac{-1}{r^2}-\frac{2 \lambda'}{r})$$
$$G_0^1=\frac{2\dot \lambda}{r}+e^{-\lambda-\nu}$$
$$G_1^1=\frac{-1}{r^2}+e^{-2\lambda}(\frac{1}{r^2}+\frac{2 \nu'}{r})$$
$$G_2^2=G_3^3=e^{-2\lambda}(\nu'^2-\nu'\lambda'+\nu''+\frac{\nu'-\lambda'}{r})+e^{-2\nu}(-\dot \lambda^2+\dot\lambda\dot\nu-\ddot \lambda)$$
$$G_{\nu}^{\mu}=0 \text{ elsewhere}$$
with $'=\frac{\partial}{\partial r}$ and $\dot{}=\frac{\partial}{\partial t}$.
Sorry I know maybe it is a trivial question for this iste, but I don't know how starting in order to find out the expression above...can you help me please?
 A: You have your metric ansatz:
$$g_{μν}=-e^{2\nu}dt^2+e^{2\lambda}dr^2+r^2d\Omega^2$$
where $λ=λ(t,r), ν=ν(t,r)$.
You want to compute the Einstein tensor which is defined as:
$$G_{αβ} = R_{αβ} - \cfrac{1}{2}g_{αβ}R$$
In order to compute the Einstein tensor you have to compute the Ricci tensor which is defined as:
$$R_{αβ}=Γ^{ρ}_{βα,ρ} - Γ^{ρ}_{ρα,β} +Γ^{ρ}_{ρλ}Γ^{λ}_{βα} -Γ^{ρ}_{βλ}Γ^{λ}_{ρα}$$
where the Christoffel symbols are given by:
$$Γ^{δ}_{βγ}= \frac{1}{2}g^{αδ}(\frac{\partial g_{αβ}}{\partial x^{γ}} + \frac{\partial g_{αγ}}{\partial x^{β}} - \frac{\partial g_{βγ}}{\partial x^{α}})$$
So you have at first to compute the Christoffel symbols from which you can get the expression for the Ricci tensor. Then you need to compute the Ricci scalar which is defined as:
$$R = g^{αβ}R_{αβ} = g^{tt}R_{tt} +g^{rr}R_{rr}+ g^{θθ}R_{θθ} + g^{\phi\phi}R_{\phi\phi}$$
After careful calculations you can obtain the Einstein tensor. If you want to derive the Schwarzchild solution, since the Einstein equation reads:
$$G_{αβ}=0,$$
you can trace this equation to see that the Ricci scalar vanishes so Einstein equation becomes $R_{αβ}=0$ and you can avoid unnecessary calculations.
EDIT 1: Calculation of one of the Christoffel symbols
The equation is:
$$Γ^{δ}_{βγ}= \frac{1}{2}g^{αδ}(\frac{\partial g_{αβ}}{\partial x^{γ}} + \frac{\partial g_{αγ}}{\partial x^{β}} - \frac{\partial g_{βγ}}{\partial x^{α}})$$
For $α=δ=r$ we have:
$$Γ^{r}_{βγ}= \frac{1}{2}g^{rr}(\frac{\partial g_{rβ}}{\partial x^{γ}} + \frac{\partial g_{rγ}}{\partial x^{β}} - \frac{\partial g_{βγ}}{\partial r})$$
For $β=γ=t:$
$$Γ^{r}_{tt}= \frac{1}{2}g^{rr}(\frac{\partial g_{rt}}{\partial t} + \frac{\partial g_{rt}}{\partial t} - \frac{\partial g_{tt}}{\partial r})$$
Since metric is diagonal this becomes:
$$Γ^{r}_{tt}= \frac{1}{2}g^{rr}(- \frac{\partial g_{tt}}{\partial r}) = \cfrac{1}{2}e^{-2λ(t,r)}2ν'(t,r)e^{-2ν} =ν'(t,r)e^{-2(λ+ν)}$$
You have to do the same for all possible combinations of $α,β,γ,δ$. Remember that the factor in front of the Christoffels is $g^{αδ}$ which is zero for any $α \neq δ$ so you need to check only the cases where $α=δ$. Hope this hepls!
A: From the metric coefficients, you can obtain the Christoffel symbols
\begin{align}
   \Gamma^{\alpha}_{\;\;\mu \nu}=\frac{1}{2} g^{\alpha \lambda} \left(g_{\mu \lambda,\nu}+ g_{\lambda \nu,\mu}-g_{\mu  \nu, \lambda}\right) \;,
\end{align}
which you will use to determine the components of the Ricci tensor (it's a bit tedious, but straightforward)
\begin{align}
   R_{\mu \nu} &= \Gamma^{\rho}_{\;\;\mu\nu,\rho}-\Gamma^{\rho}_{\;\;\mu\rho,\nu} +  \Gamma^{\rho}_{\;\;\lambda\rho}\Gamma^{\lambda}_{\;\;\mu\nu} - \Gamma^{\rho}_{\;\;\lambda\mu}\Gamma^{\lambda}_{\;\;\rho\nu} \;, 
\end{align}
then contract the Ricci tensor with the metric to obtain the Ricci scalar
\begin{align}
   R = g^{\mu \nu} R_{\mu \nu}
\end{align}
and finally plug in everything in
\begin{align}
   G_{\mu \nu} = R_{\mu\nu} - \frac{1}{2}R g_{\mu\nu}
\end{align}
to obtain the Einstein tensor. In vacuum, $G_{\mu \nu}=0$, but it is not in presence of matter, where we should have
\begin{align}
  G_{\mu \nu} = \frac{8\pi G}{c^4} T_{\mu \nu} \;,
\end{align}
with $T_{\mu \nu}$ the matter content of the Universe.
