If we take all the three terms together, we get the relation

(66) K_{σ} = ∂τ_{σ}^ν/∂_x__{ν} - ½ _g_^{τμ} ∂_g__{μν}/∂_x__{σ}

τ_{τ}^ν

where

(66a) τ_{σ}^ν = -F_{σα} F^{να} + 1/4 δ_{σ}^ν F_{αβ} F^{αβ}.

On account of (30) the equation (66) becomes equivalent to (57) and

(57a) when K_{σ} vanishes. Thus τ_{σ}^ν’s are the energy-components of

the electro-magnetic field. With the help of (61) and (64) we can easily

show that the energy-components of the electro-magnetic field, in the

case of the special relativity theory, give rise to the well-known

Maxwell-Poynting expressions.

We have now deduced the most general laws which the gravitation-field

and matter satisfy when we use a co-ordinate system for which √(-_g_) =

1. Thereby we achieve an important simplification in all our formulas

and calculations, without renouncing the conditions of general

covariance, as we have obtained the equations through a specialisation

of the co-ordinate system from the general covariant-equations. Still

the question is not without formal interest, whether, when the

energy-components of the gravitation-field and matter is defined in a

generalised manner without any specialisation of co-ordinates, the laws

of conservation have the form of the equation (56), and the

field-equations of gravitation hold in the form (52) or (52a); such that

on the left-hand side, we have a divergence in the usual sense, and on

the right-hand side, the sum of the energy-components of matter and

gravitation. I have found out that this is indeed the case. But I am of

opinion that the communication of my rather comprehensive work on this

subject will not pay, for nothing essentially new comes out of it.

E. §21. Newton’s theory as a first approximation.

We have already mentioned several times that the special relativity

theory is to be looked upon as a special case of the general, in which

_g__{μν}’s have constant values (4). This signifies, according to what

has been said before, a total neglect of the influence of gravitation.

We get one important approximation if we consider the case when

_g__{μν}’s differ from (4) only by small magnitudes (compared to 1)

where we can neglect small quantities of the second and higher orders

(first aspect of the approximation.)

Further it should be assumed that within the space-time region

considered, _g__{μν}’s at infinite distances (using the word infinite in

a spatial sense) can, by a suitable choice of co-ordinates, tend to the

limiting values (4); _i.e._, we consider only those gravitational fields

which can be regarded as produced by masses distributed over finite

regions.

We can assume that this approximation should lead to Newton’s theory.

For it however, it is necessary to treat the fundamental equations from

another point of view. Let us consider the motion of a particle

according to the equation (46). In the case of the special relativity

theory, the components

_dx₁_/_ds_, _dx₂_/_ds_, _dx₃_/_ds_,

can take any values. This signifies that any velocity

_v_ = √((_dx₁_/_dx₄_)² + (_dx₂_/_dx₄_)² + (_dx₃_/_dx₄_)²)

can appear which is less than the velocity of light in vacuum (_v_ < 1).

If we finally limit ourselves to the consideration of the case when _v_

is small compared to the velocity of light, it signifies that the

components

_dx₁_/_ds_, _dx₂_/_ds_, _dx₃_/_ds_,

can be treated as small quantities, whereas _dx₄_/_ds_ is equal to 1, up

to the second-order magnitudes (the second point of view for

approximation).

Now we see that, according to the first view of approximation, the

magnitudes γ_{μν}^τ’s are all small quantities of at least the first

order. A glance at (46) will also show, that in this equation according

to the second view of approximation, we are only to take into account

those terms for which μ = ν = 4.

By limiting ourselves only to terms of the lowest order we get instead

of (46), first, the equations:—

_d²__x__{τ}/_dt²_ = Γ₄₄^τ, where _ds_ = _dx₄_ = _dt_,

or by limiting ourselves only to those terms which according to the

first stand-point are approximations of the first order,

$$ \frac{d^2 x_{\tau}}{dt^2} = \begin{bmatrix}44\\\tau\end{bmatrix} $$

(\tau = 1, 2, 3)

$$ \frac{d^2 x_{4}}{dt^2} = - \begin{bmatrix}4^4\\4\end{bmatrix] $$

If we further assume that the gravitation-field is quasi-static, _i.e._,

it is limited only to the case when the matter producing the

gravitation-field is moving slowly (relative to the velocity of light)

we can neglect the differentiations of the positional co-ordinates on

the right-hand side with respect to time, so that we get

(67) _d²__x__{τ}/_dt²_ = -½ ∂_g₄₄_/∂_x__{τ} (τ, = 1, 2, 3)

This is the equation of motion of a material point according to Newton’s

theory, where _g_₄₄/₂ plays the part of gravitational potential. The

remarkable thing in the result is that in the first-approximation of

motion of the material point, only the component _g₄₄_ of the

fundamental tensor appears.

Let us now turn to the field-equation (53). In this case, we have to

remember that the energy-tensor of matter is exclusively defined in a

narrow sense by the density ρ of matter, _i.e._, by the second member on

the right-hand side of 58 [(58a, or 58b)]. If we make the necessary

approximations, then all component vanish except

τ₄₄ = ρ = τ.

On the left-hand side of (53) the second term is an infinitesimal of the

second order, so that the first leads to the following terms in the

approximation, which are rather interesting for us:

$$ \frac{\partial}{\partial x_{1}} \begin{bmatrix}\mu\nu\\1\end{bmatrix}

+ \frac{\partial}{\partial x_{2}} \begin{bmatrix}\mu\nu\\2\end{bmatrix}

+ \frac{\partial}{\partial x_{3}} \begin{bmatrix}\mu\nu\\3\end{bmatrix}

+ \frac{\partial}{\partial x_{4}} \begin{bmatrix}\mu\nu\\4\end{bmatrix}

$$

By neglecting all differentiations with regard to time, this leads, when

μ = ν =4, to the expression

$$ - \frac{1}{2} ( \frac{\partial^2 g_{44}}{\partial x^2_{1}} +

\frac{\partial^2 g_{44}}{\partial x^2_{2}} + \frac{\partial^2

g_{44}}{\partial x^2_{3}} ) = - \frac{1}{2} V^2 g_{44} $$

The Principle of Relativity · 第 178 / 203 题