Physics:Minkowski space
In mathematical physics, Minkowski space (or Minkowski spacetime) (/mɪŋˈkɔːfski, ˈkɒf/^{[1]}) is a combination of threedimensional Euclidean space and time into a fourdimensional manifold where the spacetime interval between any two events is independent of the inertial frame of reference in which they are recorded. Although initially developed by mathematician Hermann Minkowski for Maxwell's equations of electromagnetism, the mathematical structure of Minkowski spacetime was shown to be implied by the postulates of special relativity.^{[2]}
Minkowski space is closely associated with Einstein's theories of special relativity and general relativity and is the most common mathematical structure on which special relativity is formulated. While the individual components in Euclidean space and time may differ due to length contraction and time dilation, in Minkowski spacetime, all frames of reference will agree on the total distance in spacetime between events.^{[nb 1]} Because it treats time differently than it treats the 3 spatial dimensions, Minkowski space differs from fourdimensional Euclidean space.
In 3dimensional Euclidean space (e.g., simply space in Galilean relativity), the isometry group (the maps preserving the regular Euclidean distance) is the Euclidean group. It is generated by rotations, reflections and translations. When time is amended as a fourth dimension, the further transformations of translations in time and Galilean boosts are added, and the group of all these transformations is called the Galilean group. All Galilean transformations preserve the 3dimensional Euclidean distance. This distance is purely spatial. Time differences are separately preserved as well. This changes in the spacetime of special relativity, where space and time are interwoven.
Spacetime is equipped with an indefinite nondegenerate bilinear form, variously called the Minkowski metric,^{[3]} the Minkowski norm squared or Minkowski inner product depending on the context.^{[nb 2]} The Minkowski inner product is defined so as to yield the spacetime interval between two events when given their coordinate difference vector as argument.^{[4]} Equipped with this inner product, the mathematical model of spacetime is called Minkowski space. The analogue of the Galilean group for Minkowski space, preserving the spacetime interval (as opposed to the spatial Euclidean distance) is the Poincaré group.
As manifolds, Galilean spacetime and Minkowski spacetime are the same. They differ in what further structures are defined on them. The former has the Euclidean distance function and time interval (separately) together with inertial frames whose coordinates are related by Galilean transformations, while the latter has the Minkowski metric together with inertial frames whose coordinates are related by Poincaré transformations.
History
Part of a series on 
Spacetime 

Special relativity General relativity 
Complex Minkowski spacetime
In his second relativity paper in 1905–06 Henri Poincaré showed^{[5]} how, by taking time to be an imaginary fourth spacetime coordinate ict, where c is the speed of light and i is the imaginary unit, Lorentz transformations can be visualized as ordinary rotations of the four dimensional Euclidean sphere [math]\displaystyle{ x^2 + y^2 + z^2 + (ict)^2 = \text{const}. }[/math]
Poincaré set c = 1 for convenience. Rotations in planes spanned by two space unit vectors appear in coordinate space as well as in physical spacetime as Euclidean rotations and are interpreted in the ordinary sense. The "rotation" in a plane spanned by a space unit vector and a time unit vector, while formally still a rotation in coordinate space, is a Lorentz boost in physical spacetime with real inertial coordinates. The analogy with Euclidean rotations is only partial since the radius of the sphere is actually imaginary which turns rotations into rotations in hyperbolic space. (see hyperbolic rotation)
This idea, which was mentioned only very briefly by Poincaré, was elaborated in great detail by Minkowski in an extensive and influential paper in German in 1908 called "The Fundamental Equations for Electromagnetic Processes in Moving Bodies".^{[6]} Minkowski, using this formulation, restated the thenrecent theory of relativity of Einstein. In particular, by restating the Maxwell equations as a symmetrical set of equations in the four variables (x, y, z, ict) combined with redefined vector variables for electromagnetic quantities, he was able to show directly and very simply their invariance under Lorentz transformation. He also made other important contributions and used matrix notation for the first time in this context. From his reformulation he concluded that time and space should be treated equally, and so arose his concept of events taking place in a unified fourdimensional spacetime continuum.
Real Minkowski spacetime
In a further development in his 1908 "Space and Time" lecture,^{[7]} Minkowski gave an alternative formulation of this idea that used a real time coordinate instead of an imaginary one, representing the four variables (x, y, z, t) of space and time in coordinate form in a four dimensional real vector space. Points in this space correspond to events in spacetime. In this space, there is a defined lightcone associated with each point, and events not on the lightcone are classified by their relation to the apex as spacelike or timelike. It is principally this view of spacetime that is current nowadays, although the older view involving imaginary time has also influenced special relativity.
In the English translation of Minkowski's paper, the Minkowski metric as defined below is referred to as the line element. The Minkowski inner product of below appears unnamed when referring to orthogonality (which he calls normality) of certain vectors, and the Minkowski norm squared is referred to (somewhat cryptically, perhaps this is translation dependent) as "sum".
Minkowski's principal tool is the Minkowski diagram, and he uses it to define concepts and demonstrate properties of Lorentz transformations (e.g. proper time and length contraction) and to provide geometrical interpretation to the generalization of Newtonian mechanics to relativistic mechanics. For these special topics, see the referenced articles, as the presentation below will be principally confined to the mathematical structure (Minkowski metric and from it derived quantities and the Poincaré group as symmetry group of spacetime) following from the invariance of the spacetime interval on the spacetime manifold as consequences of the postulates of special relativity, not to specific application or derivation of the invariance of the spacetime interval. This structure provides the background setting of all present relativistic theories, barring general relativity for which flat Minkowski spacetime still provides a springboard as curved spacetime is locally Lorentzian.
Minkowski, aware of the fundamental restatement of the theory which he had made, said
The views of space and time which I wish to lay before you have sprung from the soil of experimental physics, and therein lies their strength. They are radical. Henceforth space by itself, and time by itself, are doomed to fade away into mere shadows, and only a kind of union of the two will preserve an independent reality.— Hermann Minkowski, 1908, 1909^{[7]}
Though Minkowski took an important step for physics, Albert Einstein saw its limitation:
At a time when Minkowski was giving the geometrical interpretation of special relativity by extending the Euclidean threespace to a quasiEuclidean fourspace that included time, Einstein was already aware that this is not valid, because it excludes the phenomenon of gravitation. He was still far from the study of curvilinear coordinates and Riemannian geometry, and the heavy mathematical apparatus entailed.^{[8]}
For further historical information see references (Galison 1979), (Corry 1997) and (Walter 1999).
Causal structure
Where v is velocity, and x, y, and z are Cartesian coordinates in 3dimensional space, and c is the constant representing the universal speed limit, and t is time, the fourdimensional vector v = (ct, x, y, z) = (ct, r) is classified according to the sign of c^{2}t^{2} − r^{2}. A vector is timelike if c^{2}t^{2} > r^{2}, spacelike if c^{2}t^{2} < r^{2}, and null or lightlike if c^{2}t^{2} = r^{2}. This can be expressed in terms of the sign of η(v, v) as well, which depends on the signature. The classification of any vector will be the same in all frames of reference that are related by a Lorentz transformation (but not by a general Poincaré transformation because the origin may then be displaced) because of the invariance of the interval.
The set of all null vectors at an event^{[nb 3]} of Minkowski space constitutes the light cone of that event. Given a timelike vector v, there is a worldline of constant velocity associated with it, represented by a straight line in a Minkowski diagram.
Once a direction of time is chosen,^{[nb 4]} timelike and null vectors can be further decomposed into various classes. For timelike vectors one has
 futuredirected timelike vectors whose first component is positive, (tip of vector located in absolute future in figure) and
 pastdirected timelike vectors whose first component is negative (absolute past).
Null vectors fall into three classes:
 the zero vector, whose components in any basis are (0, 0, 0, 0) (origin),
 futuredirected null vectors whose first component is positive (upper light cone), and
 pastdirected null vectors whose first component is negative (lower light cone).
Together with spacelike vectors there are 6 classes in all.
An orthonormal basis for Minkowski space necessarily consists of one timelike and three spacelike unit vectors. If one wishes to work with nonorthonormal bases it is possible to have other combinations of vectors. For example, one can easily construct a (nonorthonormal) basis consisting entirely of null vectors, called a null basis.
Vector fields are called timelike, spacelike or null if the associated vectors are timelike, spacelike or null at each point where the field is defined.
Properties of timelike vectors
Timelike vectors have special importance in the theory of relativity as they correspond to events which are accessible to the observer at (0, 0, 0, 0) with a speed less than that of light. Of most interest are timelike vectors which are similarly directed i.e.all either in the forward or in the backward cones. Such vectors have several properties not shared by spacelike vectors. These arise because both forward and backward cones are convex whereas the spacelike region is not convex.
Scalar product
The scalar product of two timelike vectors u_{1} = (t_{1}, x_{1}, y_{1}, z_{1}) and u_{2} = (t_{2}, x_{2}, y_{2}, z_{2}) is [math]\displaystyle{ \eta (u_1, u_2) = u_1 \cdot u_2 = c^2 t_1 t_2  x_1 x_2  y_1 y_2  z_1 z_2 . }[/math]
Positivity of scalar product: An important property is that the scalar product of two similarly directed timelike vectors is always positive. This can be seen from the reversed Cauchy–Schwarz inequality below. It follows that if the scalar product of two vectors is zero then one of these at least, must be spacelike. The scalar product of two spacelike vectors can be positive or negative as can be seen by considering the product of two spacelike vectors having orthogonal spatial components and times either of different or the same signs.
Using the positivity property of timelike vectors it is easy to verify that a linear sum with positive coefficients of similarly directed timelike vectors is also similarly directed timelike (the sum remains within the lightcone because of convexity).
Norm and reversed Cauchy inequality
The norm of a timelike vector u = (ct, x, y, z) is defined as [math]\displaystyle{ \left\ u \right\ = \sqrt{ \eta(u, u) } = \sqrt{c^2 t^2  x^2  y^2  z^2} }[/math]
The reversed Cauchy inequality is another consequence of the convexity of either lightcone.^{[9]} For two distinct similarly directed timelike vectors u_{1} and u_{2} this inequality is [math]\displaystyle{ \eta(u_1, u_2) \gt \left\ u_1 \right\ \left\ u_2 \right\ }[/math] or algebraically, [math]\displaystyle{ c^2 t_1 t_2  x_1 x_2  y_1 y_2  z_1 z_2 \gt \sqrt{\left(c^2 t_1^2  x_1^2  y_1^2  z_1^2\right) \left(c^2 t_2^2  x_2^2  y_2^2  z_2^2\right)} }[/math]
From this the positivity property of the scalar product can be seen.
The reversed triangle inequality
For two similarly directed timelike vectors u and w, the inequality is^{[10]} [math]\displaystyle{ \left\ u + w \right\ \ge \left\ u \right\ + \left\ w \right\, }[/math] where the equality holds when the vectors are linearly dependent.
The proof uses the algebraic definition with the reversed Cauchy inequality:^{[11]} [math]\displaystyle{ \left\ u + w \right\ ^2 = \left\ u \right\^2 + 2 \left(u, w \right) + \left\ w \right\^2 \ge \left\ u \right\ ^2 +2 \left\ u \right\ \left\ w \right\ + \left\ w \right\^2 = \left( \left\ u \right\ + \left\ w \right\ \right)^2 }[/math] The result now follows by taking the square root on both sides.
Mathematical structure
It is assumed below that spacetime is endowed with a coordinate system corresponding to an inertial frame. This provides an origin, which is necessary in order to be able to refer to spacetime as being modeled as a vector space. This is not really physically motivated in that a canonical origin ("central" event in spacetime) should exist. One can get away with less structure, that of an affine space, but this would needlessly complicate the discussion and would not reflect how flat spacetime is normally treated mathematically in modern introductory literature.
For an overview, Minkowski space is a 4dimensional real vector space equipped with a nondegenerate, symmetric bilinear form on the tangent space at each point in spacetime, here simply called the Minkowski inner product, with metric signature either (+ − − −) or (− + + +). The tangent space at each event is a vector space of the same dimension as spacetime, 4.
Tangent vectors
In practice, one need not be concerned with the tangent spaces. The vector space nature of Minkowski space allows for the canonical identification of vectors in tangent spaces at points (events) with vectors (points, events) in Minkowski space itself. See e.g. (Lee 2003) or (Lee 2012) These identifications are routinely done in mathematics. They can be expressed formally in Cartesian coordinates as^{[12]} [math]\displaystyle{ \begin{align} \left(x^0,\, x^1,\, x^2,\, x^3\right) \ &\leftrightarrow\ \left. x^0 \mathbf e_0 \right_p + \left. x^1 \mathbf e_1 \right_p + \left. x^2 \mathbf e_2 \right_p + \left. x^3 \mathbf e_3 \right_p \\ &\leftrightarrow\ \left. x^0 \mathbf e_0 \right_q + \left. x^1 \mathbf e_1 \right_q + \left. x^2 \mathbf e_2 \right_q + \left. x^3 \mathbf e_3 \right_q \end{align} }[/math] with basis vectors in the tangent spaces defined by [math]\displaystyle{ \left.\mathbf e_\mu\right_p = \left.\frac{\partial}{\partial x^\mu}\right_p \text{ or } \mathbf e_0_p = \left(\begin{matrix} 1 \\ 0 \\ 0 \\ 0\end{matrix}\right) \text{, etc}. }[/math]
Here p and q are any two events and the second basis vector identification is referred to as parallel transport. The first identification is the canonical identification of vectors in the tangent space at any point with vectors in the space itself. The appearance of basis vectors in tangent spaces as first order differential operators is due to this identification. It is motivated by the observation that a geometrical tangent vector can be associated in a onetoone manner with a directional derivative operator on the set of smooth functions. This is promoted to a definition of tangent vectors in manifolds not necessarily being embedded in R^{n}. This definition of tangent vectors is not the only possible one as ordinary ntuples can be used as well.
A tangent vector at a point p may be defined, here specialized to Cartesian coordinates in Lorentz frames, as 4 × 1 column vectors v associated to each Lorentz frame related by Lorentz transformation Λ such that the vector v in a frame related to some frame by Λ transforms according to v → Λv. This is the same way in which the coordinates x^{μ} transform. Explicitly, [math]\displaystyle{ \begin{align} x'^\mu &= {\Lambda^\mu}_\nu x^\nu, \\ v'^\mu &= {\Lambda^\mu}_\nu v^\nu. \end{align} }[/math]
This definition is equivalent to the definition given above under a canonical isomorphism.
For some purposes it is desirable to identify tangent vectors at a point p with displacement vectors at p, which is, of course, admissible by essentially the same canonical identification.^{[13]} The identifications of vectors referred to above in the mathematical setting can correspondingly be found in a more physical and explicitly geometrical setting in (Misner Thorne). They offer various degree of sophistication (and rigor) depending on which part of the material one chooses to read.
Metric signature
The metric signature refers to which sign the Minkowski inner product yields when given space (spacelike to be specific, defined further down) and time basis vectors (timelike) as arguments. Further discussion about this theoretically inconsequential, but practically necessary, choice for purposes of internal consistency and convenience is deferred to the hide box below.
In general, but with several exceptions, mathematicians and general relativists prefer spacelike vectors to yield a positive sign, (− + + +), while particle physicists tend to prefer timelike vectors to yield a positive sign, (+ − − −). Authors covering several areas of physics, e.g. Steven Weinberg and Landau and Lifshitz ((− + + +) and (+ − − −) respectively) stick to one choice regardless of topic. Arguments for the former convention include "continuity" from the Euclidean case corresponding to the nonrelativistic limit c → ∞. Arguments for the latter include that minus signs, otherwise ubiquitous in particle physics, go away. Yet other authors, especially of introductory texts, e.g. (Kleppner Kolenkow), do not choose a signature at all, but instead opt to coordinatize spacetime such that the time coordinate (but not time itself!) is imaginary. This removes the need of the explicit introduction of a metric tensor (which may seem as an extra burden in an introductory course), and one needs not be concerned with covariant vectors and contravariant vectors (or raising and lowering indices) to be described below. The inner product is instead effected by a straightforward extension of the dot product in R^{3} to R^{3} × C. This works in the flat spacetime of special relativity, but not in the curved spacetime of general relativity, see (Misner Thorne) (who, by the way use (− + + +)). MTW also argues that it hides the true indefinite nature of the metric and the true nature of Lorentz boosts, which aren't rotations. It also needlessly complicates the use of tools of differential geometry that are otherwise immediately available and useful for geometrical description and calculation – even in the flat spacetime of special relativity, e.g. of the electromagnetic field.
Terminology
Mathematically associated to the bilinear form is a tensor of type (0,2) at each point in spacetime, called the Minkowski metric.^{[nb 5]} The Minkowski metric, the bilinear form, and the Minkowski inner product are all the same object; it is a bilinear function that accepts two (contravariant) vectors and returns a real number. In coordinates, this is the 4×4 matrix representing the bilinear form.
For comparison, in general relativity, a Lorentzian manifold L is likewise equipped with a metric tensor g, which is a nondegenerate symmetric bilinear form on the tangent space T_{p}L at each point p of L. In coordinates, it may be represented by a 4×4 matrix depending on spacetime position. Minkowski space is thus a comparatively simple special case of a Lorentzian manifold. Its metric tensor is in coordinates the same symmetric matrix at every point of M, and its arguments can, per above, be taken as vectors in spacetime itself.
Introducing more terminology (but not more structure), Minkowski space is thus a pseudoEuclidean space with total dimension n = 4 and signature (3, 1) or (1, 3). Elements of Minkowski space are called events. Minkowski space is often denoted R^{3,1} or R^{1,3} to emphasize the chosen signature, or just M. It is perhaps the simplest example of a pseudoRiemannian manifold.
Then mathematically, the metric is a bilinear form on an abstract fourdimensional real vector space [math]\displaystyle{ V }[/math], that is,
 [math]\displaystyle{ \eta:V\times V\rightarrow \mathbb{R} }[/math]
where [math]\displaystyle{ \eta }[/math] has signature [math]\displaystyle{ (,+,+,+) }[/math], and signature is a coordinateinvariant property of [math]\displaystyle{ \eta }[/math]. The space of bilinear maps forms a vector space which can be identified with [math]\displaystyle{ M^*\otimes M^* }[/math], and [math]\displaystyle{ \eta }[/math] may be equivalently viewed as an element of this space. By making a choice of orthonormal basis [math]\displaystyle{ \{e_\mu\} }[/math], we can identify [math]\displaystyle{ M:=(V,\eta) }[/math] with the space [math]\displaystyle{ \mathbb{R}^{1,3}:=(\mathbb{R}^{4},\eta_{\mu\nu}) }[/math]. The notation is meant to emphasise the fact that [math]\displaystyle{ M }[/math] and [math]\displaystyle{ \mathbb{R}^{1,3} }[/math] are not just vector spaces but have added structure. [math]\displaystyle{ \eta_{\mu\nu} = \text{diag}(1, +1, +1, +1) }[/math].
An interesting example of noninertial coordinates for (part of) Minkowski spacetime are the Born coordinates. Another useful set of coordinates are the lightcone coordinates.
PseudoEuclidean metrics
The Minkowski inner product is not an inner product, since it is not positivedefinite, i.e. the quadratic form η(v, v) need not be positive for nonzero v. The positivedefinite condition has been replaced by the weaker condition of nondegeneracy. The bilinear form is said to be indefinite. The Minkowski metric η is the metric tensor of Minkowski space. It is a pseudoEuclidean metric, or more generally a constant pseudoRiemannian metric in Cartesian coordinates. As such it is a nondegenerate symmetric bilinear form, a type (0, 2) tensor. It accepts two arguments u_{p}, v_{p}, vectors in T_{p}M, p ∈ M, the tangent space at p in M. Due to the abovementioned canonical identification of T_{p}M with M itself, it accepts arguments u, v with both u and v in M.
As a notational convention, vectors v in M, called 4vectors, are denoted in italics, and not, as is common in the Euclidean setting, with boldface v. The latter is generally reserved for the 3vector part (to be introduced below) of a 4vector.
The definition ^{[14]} [math]\displaystyle{ u \cdot v = \eta(u,\, v) }[/math] yields an inner productlike structure on M, previously and also henceforth, called the Minkowski inner product, similar to the Euclidean inner product, but it describes a different geometry. It is also called the relativistic dot product. If the two arguments are the same, [math]\displaystyle{ u \cdot u = \eta(u, u) \equiv \u\^2 \equiv u^2, }[/math] the resulting quantity will be called the Minkowski norm squared. The Minkowski inner product satisfies the following properties.
 Linearity in first argument
 [math]\displaystyle{ \eta(au + v,\, w) = a\eta(u,\, w) + \eta(v,\, w),\quad \forall u,\, v \in M,\; \forall a \in \R }[/math]
 Symmetry
 [math]\displaystyle{ \eta(u,\, v) = \eta(v,\, u) }[/math]
 Nondegeneracy
 [math]\displaystyle{ \eta(u,\, v) = 0,\; \forall v \in M\ \Rightarrow\ u = 0 }[/math]
The first two conditions imply bilinearity. The defining difference between a pseudoinner product and an inner product proper is that the former is not required to be positive definite, that is, η(u, u) < 0 is allowed.
The most important feature of the inner product and norm squared is that these are quantities unaffected by Lorentz transformations. In fact, it can be taken as the defining property of a Lorentz transformation that it preserves the inner product (i.e. the value of the corresponding bilinear form on two vectors). This approach is taken more generally for all classical groups definable this way in classical group. There, the matrix Φ is identical in the case O(3, 1) (the Lorentz group) to the matrix η to be displayed below.
Two vectors v and w are said to be orthogonal if η(v, w) = 0. For a geometric interpretation of orthogonality in the special case when η(v, v) ≤ 0 and η(w, w) ≥ 0 (or vice versa), see hyperbolic orthogonality.
For a given inertial frame, an orthonormal basis in space, combined with the unit time vector, forms an orthonormal basis in Minkowski space. The number of positive and negative unit vectors in any such basis is a fixed pair of numbers, equal to the signature of the bilinear form associated with the inner product. This is Sylvester's law of inertia.
More terminology (but not more structure): The Minkowski metric is a pseudoRiemannian metric, more specifically, a Lorentzian metric, even more specifically, the Lorentz metric, reserved for 4dimensional flat spacetime with the remaining ambiguity only being the signature convention.
Minkowski metric
From the second postulate of special relativity, together with homogeneity of spacetime and isotropy of space, it follows that the spacetime interval between two arbitrary events called 1 and 2 is:^{[15]} [math]\displaystyle{ c^2\left(t_1  t_2\right)^2  \left(x_1  x_2\right)^2  \left(y_1  y_2\right)^2  \left(z_1  z_2\right)^2. }[/math]
This quantity is not consistently named in the literature. The interval is sometimes referred to as the square root of the interval as defined here.^{[16]}^{[17]}
The invariance of the interval under coordinate transformations between inertial frames follows from the invariance of [math]\displaystyle{ c^2 t^2  x^2  y^2  z^2 }[/math] provided the transformations are linear. This quadratic form can be used to define a bilinear form [math]\displaystyle{ u \cdot v = c^2 t_1 t_2  x_1 x_2  y_1 y_2  z_1 z_2. }[/math] via the polarization identity. This bilinear form can in turn be written as [math]\displaystyle{ u \cdot v = u^\textsf{T}[\eta] v, }[/math] where [η] is a 4×4 matrix associated with η. While possibly confusing, it is common practice to denote [η] with just η. The matrix is read off from the explicit bilinear form as [math]\displaystyle{ \eta = \begin{pmatrix} 1 & 0 & 0 & 0 \\ 0 & 1 & 0 & 0\\ 0 & 0 & 1 & 0\\ 0 & 0 & 0 & 1 \end{pmatrix}, }[/math] and the bilinear form [math]\displaystyle{ u \cdot v = \eta(u, v), }[/math] with which this section started by assuming its existence, is now identified.
For definiteness and shorter presentation, the signature (− + + +) is adopted below. This choice (or the other possible choice) has no (known) physical implications. The symmetry group preserving the bilinear form with one choice of signature is isomorphic (under the map given here) with the symmetry group preserving the other choice of signature. This means that both choices are in accord with the two postulates of relativity. Switching between the two conventions is straightforward. If the metric tensor η has been used in a derivation, go back to the earliest point where it was used, substitute η for −η, and retrace forward to the desired formula with the desired metric signature.
Standard basis
A standard or orthonormal basis for Minkowski space is a set of four mutually orthogonal vectors {e_{0}, e_{1}, e_{2}, e_{3}} such that [math]\displaystyle{ \eta(e_0, e_0) = \eta(e_1, e_1) = \eta(e_2, e_2) = \eta(e_3, e_3) = 1 . }[/math]
These conditions can be written compactly in the form [math]\displaystyle{ \eta(e_\mu, e_\nu) = \eta_{\mu \nu}. }[/math]
Relative to a standard basis, the components of a vector v are written (v^{0}, v^{1}, v^{2}, v^{3}) where the Einstein notation is used to write v = v^{μ} e_{μ}. The component v^{0} is called the timelike component of v while the other three components are called the spatial components. The spatial components of a 4vector v may be identified with a 3vector v = (v_{1}, v_{2}, v_{3}).
In terms of components, the Minkowski inner product between two vectors v and w is given by [math]\displaystyle{ \eta(v, w) = \eta_{\mu \nu} v^\mu w^\nu = v^0 w_0 + v^1 w_1 + v^2 w_2 + v^3 w_3 = v^\mu w_\mu = v_\mu w^\mu, }[/math] and [math]\displaystyle{ \eta(v, v) = \eta_{\mu \nu} v^\mu v^\nu = v^0v_0 + v^1 v_1 + v^2 v_2 + v^3 v_3 = v^\mu v_\mu. }[/math]
Here lowering of an index with the metric was used.
There are many possible choices of standard basis obeying the condition [math]\displaystyle{ \eta(e_\mu, e_\nu) = \eta_{\mu \nu}. }[/math] Any two such bases are related in some sense by a Lorentz transformation, either by a changeofbasis matrix [math]\displaystyle{ \Lambda^\mu_\nu }[/math], a real [math]\displaystyle{ 4\times 4 }[/math] matrix satisfying [math]\displaystyle{ \Lambda^\mu_\rho\eta_{\mu \nu}\Lambda^\nu_\sigma = \eta_{\rho \sigma}. }[/math] or [math]\displaystyle{ \Lambda, }[/math] a linear map on the abstract vector space satisfying, for any pair of vectors [math]\displaystyle{ u,v, }[/math] [math]\displaystyle{ \eta(\Lambda u, \Lambda v) = \eta(u, v). }[/math]
Then if we have two different bases [math]\displaystyle{ \{e_0,e_1,e_2,e_3\} }[/math] and [math]\displaystyle{ \{e_0',e_1',e_2',e_3'\} }[/math], we can write [math]\displaystyle{ e_\mu' = e_\nu\Lambda^\nu_\mu }[/math] or [math]\displaystyle{ e_\mu' = \Lambda e_\mu }[/math]. While it might be tempting to think of [math]\displaystyle{ \Lambda^\mu_\nu }[/math] and [math]\displaystyle{ \Lambda }[/math] as the same thing, mathematically they are elements of different spaces, and act on the space of standard bases from different sides.
Raising and lowering of indices
Technically, a nondegenerate bilinear form provides a map between a vector space and its dual; in this context, the map is between the tangent spaces of M and the cotangent spaces of M. At a point in M, the tangent and cotangent spaces are dual vector spaces (so the dimension of the cotangent space at an event is also 4). Just as an authentic inner product on a vector space with one argument fixed, by Riesz representation theorem, may be expressed as the action of a linear functional on the vector space, the same holds for the Minkowski inner product of Minkowski space.^{[19]}
Thus if v^{μ} are the components of a vector in a tangent space, then η_{μν} v^{μ} = v_{ν} are the components of a vector in the cotangent space (a linear functional). Due to the identification of vectors in tangent spaces with vectors in M itself, this is mostly ignored, and vectors with lower indices are referred to as covariant vectors. In this latter interpretation, the covariant vectors are (almost always implicitly) identified with vectors (linear functionals) in the dual of Minkowski space. The ones with upper indices are contravariant vectors. In the same fashion, the inverse of the map from tangent to cotangent spaces, explicitly given by the inverse of η in matrix representation, can be used to define raising of an index. The components of this inverse are denoted η^{μν}. It happens that η^{μν} = η_{μν}. These maps between a vector space and its dual can be denoted η^{♭} (etaflat) and η^{♯} (etasharp) by the musical analogy.^{[20]}
Contravariant and covariant vectors are geometrically very different objects. The first can and should be thought of as arrows. A linear functional can be characterized by two objects: its kernel, which is a hyperplane passing through the origin, and its norm. Geometrically thus, covariant vectors should be viewed as a set of hyperplanes, with spacing depending on the norm (bigger = smaller spacing), with one of them (the kernel) passing through the origin. The mathematical term for a covariant vector is 1covector or 1form (though the latter is usually reserved for covector fields).
(Misner Thorne) uses a vivid analogy with wave fronts of a de Broglie wave (scaled by a factor of Planck's reduced constant) quantum mechanically associated to a momentum fourvector to illustrate how one could imagine a covariant version of a contravariant vector. The inner product of two contravariant vectors could equally well be thought of as the action of the covariant version of one of them on the contravariant version of the other. The inner product is then how many time the arrow pierces the planes. The mathematical reference, (Lee 2003), offers the same geometrical view of these objects (but mentions no piercing).
The electromagnetic field tensor is a differential 2form, which geometrical description can as well be found in MTW.
One may, of course, ignore geometrical views all together (as is the style in e.g. (Weinberg 2002) and Landau & Lifshitz 2002) and proceed algebraically in a purely formal fashion. The timeproven robustness of the formalism itself, sometimes referred to as index gymnastics, ensures that moving vectors around and changing from contravariant to covariant vectors and vice versa (as well as higher order tensors) is mathematically sound. Incorrect expressions tend to reveal themselves quickly.
Coordinate free raising and lowering
Given a bilinear form [math]\displaystyle{ \eta:M\times M\rightarrow \mathbb{R} }[/math], the lowered version of a vector can be thought of as the partial evaluation of [math]\displaystyle{ \eta }[/math], that is, there is an associated partial evaluation map
 [math]\displaystyle{ \eta(\cdot, ):M\rightarrow M^*; v \mapsto \eta(v,\cdot). }[/math]
The lowered vector [math]\displaystyle{ \eta(v,\cdot)\in M^* }[/math] is then the dual map [math]\displaystyle{ u\mapsto\eta(v,u) }[/math]. Note it does not matter which argument is partially evaluated due to symmetry of [math]\displaystyle{ \eta }[/math].
Nondegeneracy is then equivalent to injectivity of the partial evaluation map, or equivalently nondegeneracy tells us the kernel of the map is trivial. In finite dimension, as we have here, and noting that the dimension of a finite dimensional space is equal to the dimension of the dual, this is enough to conclude the partial evaluation map is a linear isomorphism from [math]\displaystyle{ M }[/math] to [math]\displaystyle{ M^* }[/math]. This then allows definition of the inverse partial evaluation map,
 [math]\displaystyle{ \eta^{1}:M^*\rightarrow M, }[/math]
which allows us to define the inverse metric
 [math]\displaystyle{ \eta^{1}:M^*\times M^* \rightarrow \mathbb{R}, \eta^{1}(\alpha,\beta) = \eta(\eta^{1}(\alpha),\eta^{1}(\beta)) }[/math]
where the two different usages of [math]\displaystyle{ \eta^{1} }[/math] can be told apart by the argument each is evaluated on. This can then be used to raise indices. If we work in a coordinate basis, we find that the metric [math]\displaystyle{ \eta^{1} }[/math] is indeed the matrix inverse to [math]\displaystyle{ \eta. }[/math]
The formalism of the Minkowski metric
The present purpose is to show semirigorously how formally one may apply the Minkowski metric to two vectors and obtain a real number, i.e. to display the role of the differentials, and how they disappear in a calculation. The setting is that of smooth manifold theory, and concepts such as convector fields and exterior derivatives are introduced.
A fullblown version of the Minkowski metric in coordinates as a tensor field on spacetime has the appearance [math]\displaystyle{ \eta_{\mu\nu} dx^\mu \otimes dx^\nu = \eta_{\mu\nu} dx^\mu \odot dx^\nu = \eta_{\mu\nu} dx^\mu dx^\nu. }[/math]
Explanation: The coordinate differentials are 1form fields. They are defined as the exterior derivative of the coordinate functions x^{μ}. These quantities evaluated at a point p provide a basis for the cotangent space at p. The tensor product (denoted by the symbol ⊗) yields a tensor field of type (0, 2), i.e. the type that expects two contravariant vectors as arguments. On the right hand side, the symmetric product (denoted by the symbol ⊙ or by juxtaposition) has been taken. The equality holds since, by definition, the Minkowski metric is symmetric.^{[21]} The notation on the far right is also sometimes used for the related, but different, line element. It is not a tensor. For elaboration on the differences and similarities, see (Misner Thorne)
Tangent vectors are, in this formalism, given in terms of a basis of differential operators of the first order, [math]\displaystyle{ \left.\frac{\partial}{\partial x^\mu}\right_p, }[/math] where p is an event. This operator applied to a function f gives the directional derivative of f at p in the direction of increasing x^{μ} with x^{ν}, ν ≠ μ fixed. They provide a basis for the tangent space at p.
The exterior derivative df of a function f is a covector field, i.e. an assignment of a cotangent vector to each point p, by definition such that [math]\displaystyle{ df(X) = Xf, }[/math] for each vector field X. A vector field is an assignment of a tangent vector to each point p. In coordinates X can be expanded at each point p in the basis given by the ∂/∂x^{ν}_{p}. Applying this with f = x^{μ}, the coordinate function itself, and X = ∂/∂x^{ν}, called a coordinate vector field, one obtains [math]\displaystyle{ dx^\mu\left(\frac{\partial}{\partial x^\nu}\right) = \frac{\partial x^\mu}{\partial x^\nu} = \delta_\nu^\mu. }[/math]
Since this relation holds at each point p, the dx^{μ}_{p} provide a basis for the cotangent space at each p and the bases dx^{μ}_{p} and ∂/∂x^{ν}_{p} are dual to each other, [math]\displaystyle{ \left. dx^\mu \right_p \left(\left.\frac{\partial}{\partial x^\nu}\right_p\right) = \delta^\mu_\nu. }[/math] at each p. Furthermore, one has [math]\displaystyle{ \alpha \otimes \beta(a, b) = \alpha(a)\beta(b) }[/math] for general oneforms on a tangent space α, β and general tangent vectors a, b. (This can be taken as a definition, but may also be proved in a more general setting.)
Thus when the metric tensor is fed two vectors fields a, b, both expanded in terms of the basis coordinate vector fields, the result is [math]\displaystyle{ \eta_{\mu\nu} dx^\mu \otimes dx^\nu(a, b) = \eta_{\mu\nu} a^\mu b^\nu, }[/math] where a^{μ}, b^{ν} are the component functions of the vector fields. The above equation holds at each point p, and the relation may as well be interpreted as the Minkowski metric at p applied to two tangent vectors at p.
As mentioned, in a vector space, such as that modelling the spacetime of special relativity, tangent vectors can be canonically identified with vectors in the space itself, and vice versa. This means that the tangent spaces at each point are canonically identified with each other and with the vector space itself. This explains how the right hand side of the above equation can be employed directly, without regard to spacetime point the metric is to be evaluated and from where (which tangent space) the vectors come from.
This situation changes in general relativity. There one has [math]\displaystyle{ g(p)_{\mu\nu} \left. dx^\mu \right_p \left. dx^\nu \right_p(a, b) = g(p)_{\mu\nu} a^\mu b^\nu, }[/math] where now η → g(p), i.e., g is still a metric tensor but now depending on spacetime and is a solution of Einstein's field equations. Moreover, a, b must be tangent vectors at spacetime point p and can no longer be moved around freely.
Chronological and causality relations
Let x, y ∈ M. We say that
 x chronologically precedes y if y − x is futuredirected timelike. This relation has the transitive property and so can be written x < y.
 x causally precedes y if y − x is futuredirected null or futuredirected timelike. It gives a partial ordering of spacetime and so can be written x ≤ y.
Suppose x ∈ M is timelike. Then the simultaneous hyperplane for x is [math]\displaystyle{ \{y : \eta(x, y) = 0\}. }[/math] Since this hyperplane varies as x varies, there is a relativity of simultaneity in Minkowski space.
Generalizations
A Lorentzian manifold is a generalization of Minkowski space in two ways. The total number of spacetime dimensions is not restricted to be 4 (2 or more) and a Lorentzian manifold need not be flat, i.e. it allows for curvature.
Complexified Minkowski space
Complexified Minkowski space is defined as M_{c} = M ⊕ iM.^{[22]} Its real part is the Minkowski space of fourvectors, such as the fourvelocity and the fourmomentum, which are independent of the choice of orientation of the space. The imaginary part, on the other hand, may consist of fourpseudovectors, such as angular velocity and magnetic moment, which change their direction with a change of orientation. We introduce a pseudoscalar i which also changes sign with a change of orientation. Thus, elements of M_{c} are independent of the choice of the orientation.
The inner productlike structure on M_{c} is defined as u ⋅ v = η(u,v) for any u,v ∈ M_{c}. A relativistic pure spin of an electron or any half spin particle is described by ρ ∈ M_{c} as ρ = u+is, where u is the fourvelocity of the particle, satisfying u^{2} = 1 and s is the 4D spin vector,^{[23]} which is also the Pauli–Lubanski pseudovector satisfying s^{2} = −1 and u⋅s = 0.
Generalized Minkowski space
Minkowski space refers to a mathematical formulation in four dimensions. However, the mathematics can easily be extended or simplified to create an analogous generalized Minkowski space in any number of dimensions. If n ≥ 2, ndimensional Minkowski space is a vector space of real dimension n on which there is a constant Minkowski metric of signature (n − 1, 1) or (1, n − 1). These generalizations are used in theories where spacetime is assumed to have more or less than 4 dimensions. String theory and Mtheory are two examples where n > 4. In string theory, there appears conformal field theories with 1 + 1 spacetime dimensions.
de Sitter space can be formulated as a submanifold of generalized Minkowski space as can the model spaces of hyperbolic geometry (see below).
Curvature
As a flat spacetime, the three spatial components of Minkowski spacetime always obey the Pythagorean Theorem. Minkowski space is a suitable basis for special relativity, a good description of physical systems over finite distances in systems without significant gravitation. However, in order to take gravity into account, physicists use the theory of general relativity, which is formulated in the mathematics of a nonEuclidean geometry. When this geometry is used as a model of physical space, it is known as curved space.
Even in curved space, Minkowski space is still a good description in an infinitesimal region surrounding any point (barring gravitational singularities).^{[nb 6]} More abstractly, we say that in the presence of gravity spacetime is described by a curved 4dimensional manifold for which the tangent space to any point is a 4dimensional Minkowski space. Thus, the structure of Minkowski space is still essential in the description of general relativity.
Geometry
The meaning of the term geometry for the Minkowski space depends heavily on the context. Minkowski space is not endowed with a Euclidean geometry, and not with any of the generalized Riemannian geometries with intrinsic curvature, those exposed by the model spaces in hyperbolic geometry (negative curvature) and the geometry modeled by the sphere (positive curvature). The reason is the indefiniteness of the Minkowski metric. Minkowski space is, in particular, not a metric space and not a Riemannian manifold with a Riemannian metric. However, Minkowski space contains submanifolds endowed with a Riemannian metric yielding hyperbolic geometry.
Model spaces of hyperbolic geometry of low dimension, say 2 or 3, cannot be isometrically embedded in Euclidean space with one more dimension, i.e. ℝ^{3} or ℝ^{4} respectively, with the Euclidean metric g, disallowing easy visualization.^{[nb 7]}^{[24]} By comparison, model spaces with positive curvature are just spheres in Euclidean space of one higher dimension.^{[25]} Hyperbolic spaces can be isometrically embedded in spaces of one more dimension when the embedding space is endowed with the Minkowski metric η.
Define H1(n)R ⊂ M^{n+1} to be the upper sheet (ct > 0) of the hyperboloid
 [math]\displaystyle{ \mathbf H_R^{1(n)} = \left\{\left(ct, x^1, \ldots, x^n\right) \in \mathbf M^n: c^2 t^2  \left(x^1\right)^2 \cdots \left(x^n\right)^2 = R^2, ct \gt 0\right\} }[/math]
in generalized Minkowski space M^{n+1} of spacetime dimension n + 1. This is one of the surfaces of transitivity of the generalized Lorentz group. The induced metric on this submanifold,
 [math]\displaystyle{ h_R^{1(n)} = \iota^* \eta, }[/math]
the pullback of the Minkowski metric η under inclusion, is a Riemannian metric. With this metric H1(n)R is a Riemannian manifold. It is one of the model spaces of Riemannian geometry, the hyperboloid model of hyperbolic space. It is a space of constant negative curvature −1/R^{2}.^{[26]} The 1 in the upper index refers to an enumeration of the different model spaces of hyperbolic geometry, and the n for its dimension. A 2(2) corresponds to the Poincaré disk model, while 3(n) corresponds to the Poincaré halfspace model of dimension n.
Preliminaries
In the definition above ι: H1(n)R → M^{n+1} is the inclusion map and the superscript star denotes the pullback. The present purpose is to describe this and similar operations as a preparation for the actual demonstration that H1(n)R actually is a hyperbolic space.
Behavior of tensors under inclusion, pullback of covariant tensors under general maps and pushforward of vectors under general maps 

Behavior of tensors under inclusion:
where X_{1}, X_{1}, …, X_{k} are vector fields on S. The subscript star denotes the pushforward (to be introduced later), and it is in this special case simply the identity map (as is the inclusion map). The latter equality holds because a tangent space to a submanifold at a point is in a canonical way a subspace of the tangent space of the manifold itself at the point in question. One may simply write
meaning (with slight abuse of notation) the restriction of α to accept as input vectors tangent to some s ∈ S only. Pullback of tensors under general maps:
where for any vector space V,
It is defined by
where the subscript star denotes the pushforward of the map F, and X^{1}, X^{2}, …, X^{k} are vectors in T_{p}M. (This is in accord with what was detailed about the pullback of the inclusion map. In the general case here, one cannot proceed as simply because F_{∗}X_{1} ≠ X_{1} in general.) The pushforward of vectors under general maps: Further unwinding the definitions, the pushforward F_{∗}: TM_{p} → TN_{F(p)} of a vector field under a map F: M → N between manifolds is defined by
where f is a function on N. When M = ℝ^{m}, N= ℝ^{n} the pushforward of F reduces to DF: ℝ^{m} → ℝ^{n}, the ordinary differential, which is given by the Jacobian matrix of partial derivatives of the component functions. The differential is the best linear approximation of a function F from ℝ^{m} to ℝ^{n}. The pushforward is the smooth manifold version of this. It acts between tangent spaces, and is in coordinates represented by the Jacobian matrix of the coordinate representation of the function. The corresponding pullback is the dual map from the dual of the range tangent space to the dual of the domain tangent space, i.e. it is a linear map,

Hyperbolic stereographic projection
In order to exhibit the metric it is necessary to pull it back via a suitable parametrization. A parametrization of a submanifold S of M is a map U ⊂ R^{m} → M whose range is an open subset of S. If S has the same dimension as M, a parametrization is just the inverse of a coordinate map φ: M → U ⊂ R^{m}. The parametrization to be used is the inverse of hyperbolic stereographic projection. This is illustrated in the figure to the left for n = 2. It is instructive to compare to stereographic projection for spheres.
Stereographic projection σ: HnR → R^{n} and its inverse σ^{−1}: R^{n} → HnR are given by [math]\displaystyle{ \begin{align} \sigma(\tau, \mathbf x) = \mathbf u &= \frac{R\mathbf x}{R + \tau},\\ \sigma^{1}(\mathbf u) = (\tau, \mathbf x) &= \left(R\frac{R^2 + u^2}{R^2  u^2}, \frac{2R^2\mathbf u}{R^2  u^2}\right), \end{align} }[/math] where, for simplicity, τ ≡ ct. The (τ, x) are coordinates on M^{n+1} and the u are coordinates on R^{n}.
Let
 [math]\displaystyle{ \mathbf H_R^n = \left\{\left(\tau, x^1, \ldots, x^n\right) \subset \mathbf M: \tau^2 + \left(x^1\right)^2 + \cdots + \left(x^n\right)^2 = R^2, \tau \gt 0\right\} }[/math]
and let
 [math]\displaystyle{ S = (1, 0, \ldots, 0) }[/math]
If
 [math]\displaystyle{ P = \left(\tau, x^1, \ldots, x^n\right) \in \mathbf H_R^n, }[/math]
then it is geometrically clear that the vector
 [math]\displaystyle{ \overrightarrow{PS} }[/math]
intersects the hyperplane
 [math]\displaystyle{ \left\{\left(\tau, x^1, \ldots, x^n\right) \in M: \tau = 0\right\} }[/math]
once in point denoted
 [math]\displaystyle{ U = \left(0, u^1(P), \ldots, u^n(P)\right) \equiv (0, \mathbf u). }[/math]
One has
 [math]\displaystyle{ \begin{align} S + \overrightarrow{SU} &= U \Rightarrow \overrightarrow{SU} = U  S,\\ S + \overrightarrow{SP} &= P \Rightarrow \overrightarrow{SP} = U  P \end{align}. }[/math]
or
 [math]\displaystyle{ \begin{align} \overrightarrow{SU} &= (0, \mathbf u)  (R, 0) = (R, \mathbf u),\\ \overrightarrow{SP} &= (\tau, \mathbf x)  (R, 0) = (\tau + R, \mathbf x). \end{align} }[/math]
By construction of stereographic projection one has
 [math]\displaystyle{ \overrightarrow{SU} = \lambda(\tau)\overrightarrow{SP}. }[/math]
This leads to the system of equations
 [math]\displaystyle{ \begin{align} R &= \lambda(\tau + R),\\ \mathbf u &= \lambda \mathbf x. \end{align} }[/math]
The first of these is solved for [math]\displaystyle{ \lambda }[/math] and one obtains for stereographic projection
 [math]\displaystyle{ \sigma(\tau, \mathbf x) = \mathbf u = \frac{R\mathbf x}{R + \tau}. }[/math]
Next, the inverse [math]\displaystyle{ \sigma^{1}(u) = (\tau, \mathbf x) }[/math] must be calculated. Use the same considerations as before, but now with
 [math]\displaystyle{ \begin{align} U &= (0, \mathbf u)\\ P &= (\tau(\mathbf u), \xi(\mathbf u)). \end{align} }[/math]
One gets
 [math]\displaystyle{ \begin{align} \tau &= \frac{R(1  \lambda)}{\lambda},\\ \mathbf x &= \frac{\mathbf u}{\lambda}, \end{align} }[/math]
but now with [math]\displaystyle{ \lambda }[/math] depending on [math]\displaystyle{ \mathbf u. }[/math] The condition for P lying in the hyperboloid is
 [math]\displaystyle{ \tau^2 + \mathbf u \cdot \mathbf u = \tau^2 + u^2 = R^2, }[/math]
or
 [math]\displaystyle{ \frac{R^2(1  \lambda)^2}{\lambda^2} = \frac{u^2}{\lambda^2}, }[/math]
leading to
 [math]\displaystyle{ \lambda = \frac{R^2  u^2}{2R^2}. }[/math]
With this [math]\displaystyle{ \lambda }[/math], one obtains
 [math]\displaystyle{ \sigma^{1}(\mathbf u) = (\tau, \mathbf x) = \left(R\frac{R^2 + u^2}{R^2  u^2}, \frac{2R^2\mathbf u}{R^2  u^2}\right). }[/math]
Pulling back the metric
One has
 [math]\displaystyle{ h_R^{1(n)} = \eta_{\mathbf H_R^{1(n)}} = \left(dx^1\right)^2 + \ldots + \left(dx^n\right)^2  d\tau^2 }[/math]
and the map
 [math]\displaystyle{ \sigma^{1}:\mathbb{R}^n \rightarrow \mathbf{H}_R^{1(n)};\quad \sigma^{1}(\mathbf{u}) = (\tau(\mathbf{u}),\, \mathbf{x}(\mathbf{u})) = \left(R\frac{R^2 + u^2}{R^2  u^2},\, \frac{2R^2\mathbf{u}}{R^2  u^2}\right). }[/math]
The pulled back metric can be obtained by straightforward methods of calculus;
 [math]\displaystyle{ \left.\left(\sigma^{1}\right)^* \eta\right_{\mathbf H_R^{1(n)}} = \left(dx^1(\mathbf u)\right)^2 + \ldots + \left(dx^n(\mathbf u)\right)^2  \left(d\tau(\mathbf u)\right)^2. }[/math]
One computes according to the standard rules for computing differentials (though one is really computing the rigorously defined exterior derivatives),
 [math]\displaystyle{ \begin{align} dx^1(\mathbf u) &= d\left(\frac{2R^2 u^1}{R^2  u^2}\right) = \frac{\partial}{\partial u^1}\frac{2R^2 u^1}{R^2  u^2}du^1 + \ldots + \frac{\partial}{\partial u^n}\frac{2R^2 u^1}{R^2  u^2}du^n + \frac{\partial}{\partial\tau}\frac{2R^2 u^1}{R^2  u^2}d\tau,\\ &\ \ \vdots\\ dx^n(\mathbf u) &= d\left(\frac{2R^2 u^n}{R^2  u^2}\right) = \cdots,\\ d\tau(\mathbf u) &= d\left(R\frac{R^2 + u^2}{R^2  u^2}\right) = \cdots, \end{align} }[/math]
and substitutes the results into the right hand side. This yields
 [math]\displaystyle{ \left(\sigma^{1}\right)^* h_R^{1(n)} = \frac{4R^2 \left[\left(du^1\right)^2 + \ldots + \left(du^n\right)^2\right]}{\left(R^2  u^2\right)^2} \equiv h_R^{2(n)}. }[/math]
Detailed outline of computation 

One has
and
With this one may write
from which
Summing this formula one obtains
Similarly, for τ one gets
yielding
Now add this contribution to finally get

This last equation shows that the metric on the ball is identical to the Riemannian metric h2(n)R in the Poincaré ball model, another standard model of hyperbolic geometry.
Alternative calculation using the pushforward 

The pullback can be computed in a different fashion. By definition,
In coordinates,
One has from the formula for σ^{–1}
Lastly,
and the same conclusion is reached. 
See also
Remarks
 ↑ This makes spacetime distance an invariant.
 ↑ Consistent use of the terms "Minkowski inner product", "Minkowski norm" or "Minkowski metric" is intended for the bilinear form here, since it is in widespread use. It is by no means "standard" in the literature, but no standard terminology seems to exist.
 ↑ Translate the coordinate system so that the event is the new origin.
 ↑ This corresponds to the time coordinate either increasing or decreasing when proper time for any particle increases. An application of T flips this direction.
 ↑ For comparison and motivation of terminology, take a Riemannian metric, which provides a positive definite symmetric bilinear form, i. e. an inner product proper at each point on a manifold.
 ↑ This similarity between flat and curved space at infinitesimally small distance scales is foundational to the definition of a manifold in general.
 ↑ There is an isometric embedding into ℝ^{n} according to the Nash embedding theorem ((Nash 1956)), but the embedding dimension is much higher, n = (m/2)(m + 1)(3m + 11) for a Riemannian manifold of dimension m.
Notes
 ↑ "Minkowski". Random House Webster's Unabridged Dictionary.
 ↑ Landau & Lifshitz 2002, p. 4
 ↑ Lee 1997, p. 31
 ↑ Schutz, John W. (1977). Independent Axioms for Minkowski Space–Time (illustrated ed.). CRC Press. pp. 184–185. ISBN 9780582317604. https://books.google.com/books?id=eOO1SWD17GIC. Extract of page 184
 ↑ Poincaré 1905–1906, pp. 129–176 Wikisource translation: On the Dynamics of the Electron
 ↑ Minkowski 1907–1908, pp. 53–111 *Wikisource translation: s:Translation:The Fundamental Equations for Electromagnetic Processes in Moving Bodies.
 ↑ ^{7.0} ^{7.1} Minkowski 1908–1909, pp. 75–88 Various English translations on Wikisource: "Space and Time."
 ↑ Cornelius Lanczos (1972) "Einstein's Path from Special to General Relativity", pages 5–19 of General Relativity: Papers in Honour of J. L. Synge, L. O'Raifeartaigh editor, Clarendon Press, see page 11
 ↑ See Schutz's proof p 148, also Naber p.48
 ↑ Schutz p.148, Naber p.49
 ↑ Schutz p.148
 ↑ Lee 1997, p. 15
 ↑ Lee 2003, See Lee's discussion on geometric tangent vectors early in chapter 3.
 ↑ Giulini 2008 pp. 5,6
 ↑ Sean M. Carroll (2019). Spacetime and Geometry (illustrated, herdruk ed.). Cambridge University Press. p. 7. ISBN 9781108488396. https://books.google.com/books?id=PTGdDwAAQBAJ&pg=PA7.
 ↑ Sard 1970, p. 71
 ↑ Minkowski, Landau & Lifshitz 2002, p. 4
 ↑ Misner, Thorne & Wheeler 1973
 ↑ Lee 2003. One point in Lee's proof of existence of this map needs modification (Lee deals with Riemannian metrics.). Where Lee refers to positive definiteness to show injectivity of the map, one needs instead appeal to nondegeneracy.
 ↑ Lee 2003, The tangentcotangent isomorphism p. 282.
 ↑ Lee 2003
 ↑ Y. Friedman, A Physically Meaningful Relativistic Description of the Spin State of an Electron,Symmetry 2021, 13(10), 1853; https://doi.org/10.3390/sym13101853
 ↑ Jackson, J.D., Classical Electrodynamics, 3rd ed.; John Wiley \& Sons: Hoboken, NJ, USA,1998
 ↑ Lee 1997, p. 66
 ↑ Lee 1997, p. 33
 ↑ Lee 1997
References
 Corry, L. (1997). "Hermann Minkowski and the postulate of relativity". Arch. Hist. Exact Sci. 51 (4): 273–314. doi:10.1007/BF00518231. ISSN 00039519.
 Catoni, F. (2008). Mathematics of Minkowski Space. Frontiers in Mathematics. Basel: Birkhäuser Verlag. doi:10.1007/9783764386146. ISBN 9783764386139.
 Galison, P. L. (1979). R McCormach. ed. Minkowski's Space–Time: from visual thinking to the absolute world. Historical Studies in the Physical Sciences. 10. Johns Hopkins University Press. pp. 85–121. doi:10.2307/27757388.
 Giulini D The rich structure of Minkowski space, https://arxiv.org/abs/0802.4345v1
 Kleppner, D.; Kolenkow, R. J. (1978). An Introduction to Mechanics. London: McGrawHill. ISBN 9780070350489. https://archive.org/details/introductiontome00dani.
 Landau, L.D.; Lifshitz, E.M. (2002). The Classical Theory of Fields. Course of Theoretical Physics. 2 (4th ed.). Butterworth–Heinemann. ISBN 0750627689.
 Lee, J. M. (2003). Introduction to Smooth manifolds. Springer Graduate Texts in Mathematics. 218. ISBN 9780387954486.
 Lee, J. M. (2012). Introduction to Smooth manifolds. Springer Graduate Texts in Mathematics. ISBN 9781441999818.
 Lee, J. M. (1997). Riemannian Manifolds – An Introduction to Curvature. Springer Graduate Texts in Mathematics. 176. New York · Berlin · Heidelberg: Springer Verlag. ISBN 9780387983226.
 Minkowski, Hermann (1907–1908), "Die Grundgleichungen für die elektromagnetischen Vorgänge in bewegten Körpern", Nachrichten von der Gesellschaft der Wissenschaften zu Göttingen, MathematischPhysikalische Klasse: 53–111 *Wikisource translation: The Fundamental Equations for Electromagnetic Processes in Moving Bodies
 Minkowski, Hermann (1908–1909), "Raum und Zeit", Physikalische Zeitschrift 10: 75–88 Various English translations on Wikisource: Space and Time
 Misner, Charles W.; Thorne, Kip. S.; Wheeler, John A. (1973), Gravitation, W. H. Freeman, ISBN 9780716703440
 Naber, G. L. (1992). The Geometry of Minkowski Spacetime. New York: SpringerVerlag. ISBN 9780387978482.
 Nash, J. (1956). "The Imbedding Problem for Riemannian Manifolds". Annals of Mathematics 63 (1): 20–63. doi:10.2307/1969989.
 Penrose, Roger (2005). "18 Minkowskian geometry". Road to Reality : A Complete Guide to the Laws of the Universe. Alfred A. Knopf. ISBN 9780679454434. https://archive.org/details/roadtorealitycom00penr_0.
 Poincaré, Henri (1905–1906), "Sur la dynamique de l'électron", Rendiconti del Circolo Matematico di Palermo 21: 129–176, doi:10.1007/BF03013466, https://zenodo.org/record/1428444 Wikisource translation: On the Dynamics of the Electron
 Robb A A: Optical Geometry of Motion; a New View of the Theory of Relativity Cambridge 1911, (Heffers). http://www.archive.org/details/opticalgeometryoOOrobbrich
 Robb A A: Geometry of Time and Space, 1936 Cambridge Univ Press http://www.archive.org/details/geometryoftimean032218mbp
 Sard, R. D. (1970). Relativistic Mechanics  Special Relativity and Classical Particle Dynamics. New York: W. A. Benjamin. ISBN 9780805384918. https://archive.org/details/relativisticmech0000sard.
 Shaw, R. (1982). "§ 6.6 Minkowski space, § 6.7,8 Canonical forms pp 221–242". Linear Algebra and Group Representations. Academic Press. ISBN 9780126392012. https://archive.org/details/linearalgebragro0000shaw.
 Walter, Scott A. (1999). "Minkowski, Mathematicians, and the Mathematical Theory of Relativity". in Goenner, Hubert. The Expanding Worlds of General Relativity. Boston: Birkhäuser. pp. 45–86. ISBN 9780817640606. http://scottwalter.free.fr/papers/1999mmmwalter.html.
 Weinberg, S. (2002), The Quantum Theory of Fields, 1, Cambridge University Press, ISBN 9780521550017, https://archive.org/details/quantumtheoryoff00stev
External links
 Animation clip on YouTube visualizing Minkowski space in the context of special relativity.
 The Geometry of Special Relativity: The Minkowski Space  Time Light Cone
 Minkowski space at PhilPapers
Original source: https://en.wikipedia.org/wiki/Minkowski space.
Read more 