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So far we have seen how free particles move in spacetime, and it led us to the concept of geodesic. But we have to understand in more details how these two concepts are related.
We recall that the geodesic equation for a particule with mass is
As we know that in General Relativity gravity is equivalent to spacetime curvature , can we then affirm that if all the Christoffel symbols are null, then spacetime is flat, as we have verified in our article Geodesic exercise part I: calculation for 2dimensional Euclidean space for a twodimensional Euclidean space  in which geodesics are straight lines?
2surface Gaussian curvature
In fact, what we are looking for is the generalization for the fourdimensional spacetime of the twodimensional Gaussian curvature, e.g a way of determining the intrinsic measure of curvature, depending only on distances that are measured on the surface, not on the way it is embedded in any space.
If you take a flat piece of paper and bend it gently, it bends in only one direction at a time. At any point on the paper, you can find at least one direction through which there is a straight line on the surface. You can bend it into a cylinder, or into a cone, but you can never bend it without crumpling or distorting to the get a portion of the surface of a sphere.
In Gaussian terms, the cyclinder curvature  defined as the product K_{1}K_{2 } of the two principal curvatures  is null because one of these principals  the one along the axis of the cylinder  is null.
In this article, we want to find a test similar to the piece of paper bending used in two dimensions.
In fourdimensional spacetime, the test will be to try to transform a general metric g_{μν} to the Minkowski form η_{μν} by an appropriate coordinate transformation x^{μ} > x'^{μ}
From our previous article Generalisation of the metric tensor in pseudoRiemannian manifold, we know that the metric g_{μν} has 10 independant components (16  6 as the tensor is symmetric.
Also concerning the coordinate transformation x^{α } > x'^{α }, we have the choice to find a function which relates x'^{α } to (x^{0}, x^{1},x^{2} and x^{3}) for each value 0,1,2 and 3 of α.
So we have 4 degrees of freedom to fill 10 conditions, which is generally not possible: as expected, it is generally impossible to reduce a metric describing a curved spacetime to the one of a flat spacetime by a coordinate transformation.
Local Inertial Frame

Local Flatness or Local Inertial Frame (LIF)
It appears that we have to be less ambitious and try to find a primed coordinate system that locally only , i.e around a event P in spacetime
  could reduce the metric g'_{μν} in P to the Minkowski flat spacetime metric η_{μν}
  and for which all the first derivatives of the metric g'_{μν} are zero
If we take the analogy of the curved surface of the earth, we have to isolate lots of little square patches, each patch being pretty near flat.
We recall from our article Generalisation of the metric tensor in pseudoRiemannian manifold that an arbitrary metric could be expressed as:
and more generally that the components of a metric tensor in primed coordinate system could be expressed in non primed coordinates as:
Each of the partial derivatives is a function of the primed coordinates so, for a region close to the event point P, we can expand these derivatives in Taylor series:
where
These three quantities represent constant coefficients that we are allowed to choose freely in order to find a local inertial frame around the event P.
Let's try to count the degrees of freedrom we have at each step of this Taylor series development.
In the case of the coefficient a_{μ}^{α}, we can freely choose the 16 coefficients (4 possible values for α x 4 possible values for μ).
Concerning the coefficient b_{μν}^{α}, we have still 4 possible values for α but only 10 possible distinct choices over 16 for μ and ν as the order of the partial derivatives doesn’t matter here (for example, δ^{2}x^{α}/δx'^{1}δx'^{2} = δ^{2}x^{α}/δx'^{2}δx'^{1}^{[1]}). There are then 4x10 = 40 values for b_{μν}^{α }that we can freely choose.
When it comes to c_{μνβ}^{α}, again the order of the 3 partial derivatives doesn’t matter, so for each value of α we can have μ=ν=β, or two indices equal with the third different, or all three indices different. We have then to calculate the number of times that each possibility (0,1,2,3) appears in the triplet (μ,ν,β): by example in the case of the three following combinations c^{1}_{023} = c^{1}_{032} = c^{1}_{302}, we would say that they are all equivalent to one time 0, one time 1 and one time 2. This could represented with the notation xxx where the first case represents the number 0, the second case represents the number 1 and the third one represents the number 2. Another example would be the three distinct coefficients c^{1}_{002} = c^{1}_{020} = c^{1}_{200} which would be represented in a unique way by as xxx (2 number zero in the first case, 0 number 1 in the second case and 1 number 2 in the last case). The number of independants coefficients c_{μνβ}^{α} is then obtained by the number of possible unordererd permutations of three x and N1 symbols  in N+2 cases, which is by definition (N+2)!/(3! x (N1)!) = (N+2)(N+1)N/6.
As α can take N values, we finally get the number of possibilities = (N+2)(N+1)N^{2}/6 so for N=4, we get the number of independant coefficients c_{μνβ}^{α} = 16x5 = 80 values.We can also think of the unprimed metric as a function of the primed coordinates, and expand it in a Taylor series as well:
We can now substitute the product of the partial derivatives with the non primed metric into one and collect terms. Due to the large number of indices floating about, it’s easier to use a condensed notation for this step.
The transformation now becomes, up to second order terms:
If we are finally expanding the Taylor expansion of g(x'_{p} + Δ'x) where every factor is now a function of x', we get:
We therefore have, taking each term separately and restoring the indices:
As we have seen above, every choice of the two indices α and μ gives an independent quantity, so there are 16 different variables and thus we have 6 more degrees of freedom than we need to solve g'_{μν} = η_{μν }( η_{μν } being symetric only requires 10 independant coefficients).
Again, as g'_{μν} is symmetric, we have 10 distinct values which have to be mutlitplied by the 4 distinct values of the partial derivative, which gives 40 independant equations. Do we have enough freedom degrees to verify that d'_{γ}g'_{μν} = 0 around the point P?
Recalling from above that there are then 4x10 = 40 values for b_{μν}^{α }that we can freely choose, we just enough degrees of freedom to fill this condition.
We then have just defined what is called a Local Inertial Frame (LIF): mathematically, it is a coordinate frame in which the metric is locally equivalent to the Minkowski metric and for which we impose the constraint that all the derivatives of the metric are locally equal to zero. Physically, that's the free falling referential from our famous Equivalence Principle, in which gravity seems to disappear locally .
[1] In the case of a symmetric matrix of dimension N, we can show easily that the number of distinct values is equal to N(N+1)/2. If N=4, the number of distinct values is then (4x5)/2 = 10.
Spacetime Curvature

Introduction to Spacetime curvature
The last equations to be checked concern the second order derivatives of the metric:
Given the fact that both the metric and its partial derivatives are symmetric by swapping the indice order, this line represents actually 100 independant equations.
Once again, the values of the non primed metric and of its derivatives are given, and as we have already determined the values of different a and b, our freedom is limited to the 80 independant values of c^{α}_{μνγ} (see above for demonstration)
It means that there will remain 20 second derivatives that we will not be able to set to zero: it turns out that this is a result of the inherent or intrinsec curvature of the spacetime  so it’s not surprising that we can’t get rid of that.
We have found then a test equivalent to the K=k_{1}k_{2} gaussian curvature for fourdimensional Riemannian manifold: if the surface is curved, we can not find a frame for which all of the second derivatives of the metric could be null. And we will see in a later article that these 20 extra derivatives are precisely embedeed in an object called Riemanian tensor of fundamental importance to assess the spacetime curvature.