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In this post I am to follow DrPhysicsA’s excellent explanation (video provided at the end) and to provide some ideas myself.
I am also planning to re-write it afterwards - based on my own understanding.

# Introduction

The Einstein field equations (EFE; also known as Einstein’s equations) comprise the set of 10 equations in Albert Einstein’s general theory of relativity that describe the fundamental interaction of gravitation as a result of spacetime being curved by mass and energy. First published by Einstein in 1915 as a tensor equation, the EFE relate local spacetime curvature (expressed by the Einstein tensor) with the local energy and momentum within that spacetime (expressed by the stress–energy tensor).

First let’s take a look at these equations (why “these” ? see below):
$$R_{\mu\nu}-{\textstyle\frac12}Rg_{\mu\nu}-\Lambda g_{\mu\nu}=-\frac{8\pi G}{c^4}T_{\mu\nu}$$
where $R_{\mu \nu}$ is the Ricci curvature tensor, R is the scalar curvature, $g_{\mu nu}$ is the metric tensor, Λ is the cosmological constant, G is Newton’s gravitational constant, c is the speed of light in vacuum, and $T_{\mu \nu}$ is the stress–energy momentum tensor.

$\mu$ and $\nu$ have numbers from 0 to 3, so these tensors with indices have 4x4=16 “versions” while 6 of them are duplicates, so there are in total 10 equations.

The equations balance two things: Curvature of the spacetime on the left and mass/energy on the right. Thus some may say:

Mass tells spacetime how to curve and curved spacetime tells mass how to move.

# Metric Tensor

Say there is a field and the height of the field is $\Phi$, then the change of the height $d\Phi$ in the $x^n$ coordinator system (for e.g. if n=3 then it is a 3-D space with coordinators of $x^1, x^2 \ and \ x^3$) can be descripted as:

\begin{align} d\Phi&=\frac{\partial\Phi}{\partial x^1}dx^1+\frac{\partial\Phi}{\partial x^2}dx^2\cdots\nonumber\\ &=\sum_n{\frac{\partial\Phi}{\partial x^n}dx^n} \label{eq:1} \end{align}

Consider a $y^1$ in $y$ coordinator system, and again $x^1, x^2…etc.$ in $x$ coordinator system, then use chain rule we have
\begin{align} \frac{d\Phi}{dy^1}&=\frac{\partial\Phi}{\partial x^1}\frac{\partial x^1}{\partial y^1}+\frac{\partial\Phi}{\partial x^2}\frac{\partial x^2}{\partial y^1}\cdots\nonumber\\ &=\sum_m\frac{\partial\Phi}{\partial x^m}\frac{\partial x^m}{\partial y^1}\nonumber \end{align}
$$\begin{equation} \frac{\partial \Phi}{\partial y^n}=\sum_m{\frac{\partial\Phi}{\partial x^m}\frac{\partial x^m}{\partial y^n}} \label{eq:2} \end{equation}$$

Note: Equation \eqref{eq:2} is a collection of $n$ equations

Now we transform equation \eqref{eq:1} in a vector (rank 1 tensor) form by letting $d\Phi=V_y^n$ the change of height to be a vector in y coordinator system, and $dx^n=V_x^m$ the change of space to be a vector in x coordinator system:
$$\begin{equation} V_y^n=\sum_m{\frac{\partial y^n}{\partial x^m}V_x^m} \label{eq:3} \end{equation}$$

Now consider a rank 2 tensor, which is a combination of two vectors $T^{mn}=A^nB^n$

Substitute it into \eqref{eq:3}
\begin{align} T_y^{mn}&=A^mB^n\nonumber\\ &=\sum_{r,s}{\frac{\partial y^m}{\partial x^r}A_x^r\frac{\partial y^n}{\partial x^s}B_x^s}\nonumber\\ &=\sum_{r,s}{\frac{\partial y^m}{\partial x^r}\frac{\partial y^n}{\partial x^s}}T_x^{rs} \label{eq:4} \end{align}

Equation \eqref{eq:4} is a contravariant transformation

Note: Equation \eqref{eq:4} is now a collection of $m\times n$ functions

Similarly,
$$\begin{equation} T_{mn}(y)=\sum_{r,s}{\frac{\partial x^r}{\partial y^m}\frac{\partial x^s}{\partial y^n}T_{rs}(x)} \label{eq:5} \end{equation}$$

Equation \eqref{eq:5} is a covariant transformation

or we can use prime coordinators to avoid confusions caused by $T_y \ and \ T(y)$

Such as $$T_{mn}=\sum_{r,s}{\frac{\partial x^r}{\partial y^m}\frac{\partial x^s}{\partial y^n}T_{mn}’}$$

Now we need to discuss some Pythagoras theorem:

Usually we write it as $ds^2=\sum_n{dx^ndx^n}$ but here by introducing Kronecker delta $\delta_{mn}$ we can write it as $ds^2=\delta_{mn}\sum_{m,n}{dx^m dx^n}$, where
$$\begin{equation} \delta_{mn}=\{ \begin{array}{l} 1\cdots m=n\\ 0\cdots m\neq n \end{array}\nonumber \end{equation}$$

This can also be written in the matrix form, for e.g. in 3-D:
$$\left\langle\begin{bmatrix} 1&0&0\\ 0&1&0\\ 0&0&1\\ \end{bmatrix},(\begin{bmatrix} dx^1\\ dx^2\\ dx^3 \end{bmatrix}\otimes\begin{bmatrix} dx^1&dx^2&dx^3 \end{bmatrix})\right\rangle_F={dx^1}^2+{dx^2}^2+{dx^3}^2$$
the main point is $\delta_{mn}$ is a diagonal matrix.

Rewrite \eqref{eq:1} as $dx^m=\frac{\partial x^m}{\partial y^r}dy^r$(getting rid of the summation terms i.e. $\sum$ mark from now on) and substituting it into new Pythagoras we get:
\begin{align} ds^2&=\delta_{mn}\frac{\partial x^m}{\partial y^r}dy^r\frac{\partial x^n}{\partial y^s}dy^s\nonumber\\ &=\boxed{\delta_{mn}\frac{\partial x^m}{\partial y^r}\frac{\partial x^n}{\partial y^s}}dy^rdy^s\nonumber\\ &=g_{mn}dy^rdy^s \label{eq:6} \end{align}
Here comes metric tensor $g_{mn}$ (the boxed part in above equation)!

# Christoffel Symbol $\Gamma$

Now to discuss the relations between derivatives for two tensors ($W_{mn}(x)=V_{mn}(x)$)
\begin{align} T_{mn}(y)&=\frac{\partial x^r}{\partial y^m}\frac{\partial x^s}{\partial y^n}T_{rs}(x)\nonumber\\ &=\frac{\partial x^r}{\partial y^m}\frac{\partial x^s}{\partial y^n}\frac{\partial V_r(x)}{\partial x^s}\nonumber\\ &=\frac{\partial x^r}{\partial y^m}\frac{\partial V_r{x}}{\partial y^n}\nonumber \end{align}

\begin{align} \frac{\partial V_m(y)}{\partial y^n}&=\frac{\partial }{\partial y^n}(\frac{\partial x^r}{y^m}V_r(x))\nonumber\\ &=\frac{\partial x^r}{\partial y^m}\frac{\partial V_r(x)}{\partial y^n}+\boxed{\frac {\partial }{\partial y^n}\frac{\partial x^r}{\partial y^m}}V_r(x)\nonumber\\ &=\frac{\partial x^r}{\partial y^m}\frac{\partial V_r(x)}{\partial y^n}+\Gamma_{mn}^rV_r(x)=\nabla_nV_m \end{align}

# Curvature

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## Ricci Tensor

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## Curvature Scalar

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# Stress Energy Momentum Tensor

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# Cosmological Constant

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# Summary

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