# Page:LorentzGravitation1916.djvu/51

of the factor ${\displaystyle {\tfrac {1}{\varkappa }}}$ in (96) and (97)) these functions become proportional to ${\displaystyle \varkappa }$, so that in a feeble gravitation field they have low values.

§ 56. Because of the complicated form of equations (96) and (97), we shall confine ourselves to the calculation for some cases of ${\displaystyle {\mathfrak {t}}_{4}^{'4}}$, i.e. of the energy per unit of volume. This calculation is considerably simplified if we consider stationary fields only. Then all differential coefficients with respect to ${\displaystyle x_{4}}$ vanish, so that we have according to (96)

 ${\displaystyle {\mathfrak {t}}_{4}^{'4}={\frac {1}{2\varkappa }}\left\{-Q_{1}+\sum (abfe){\frac {\partial }{\partial x_{e}}}\left({\frac {\partial Q}{\partial g_{ab,fe}}}\right)g_{ab,f}\right\}}$ (99)

We shall work out the calculation, first for a field without gravitation and secondly for the case of an attracting spherical body in which the matter is distributed symmetrically round the centre.

If there is no gravitation field we may take for the quantities ${\displaystyle g_{ab}}$ the "normal" values. For the case of orthogonal coordinates these are given by (98). When we want to use the polar coordinates introduced into § 48 we have the corresponding formulae

 ${\displaystyle \left.{\begin{array}{c}g_{11}=-{\frac {r^{2}}{1-x_{1}^{2}}},\ g_{22}=-r^{2}\left(1-x_{1}^{2}\right),\ g_{33}=-1,\ g_{44}=c^{2},\\\\g_{ab}=0,\quad {\textrm {for}}\quad a\neq b\end{array}}\right\}}$ (100)

If, using polar coordinates, we have to do with an attracting sphere and if we take its centre as origin, we may put

 ${\displaystyle g_{11}=-{\frac {u}{1-x_{1}^{2}}},\ g_{22}=-\left(1-x_{1}^{2}\right)u,\ g_{33}=-v,\ g_{44}=w,}$ (101)

where ${\displaystyle u,v,w}$ are functions of ${\displaystyle r}$. The ${\displaystyle g_{ab}}$'s which belong to an orthogonal system of coordinates may be expressed in the same functions.

These ${\displaystyle g_{ab}}$'s are

${\displaystyle {\begin{array}{l}g_{11}=-{\frac {u}{r^{2}}}+{\frac {x_{1}^{2}}{r^{2}}}\left({\frac {u}{r^{2}}}-v\right),\ etc.\\\\g_{12}={\frac {x_{1}x_{2}}{r^{2}}}\left({\frac {u}{r^{2}}}-v\right),\ etc.\\\\g_{14}=g_{24}=g_{34}=0,\ g_{44}=w.\end{array}}}$

The "etc." means that for ${\displaystyle g_{22},g_{33}}$ we have similar expressions as for ${\displaystyle g_{11}}$ and for${\displaystyle g_{23},g_{31}}$ similar ones as for ${\displaystyle g_{12}}$.

§ 57. In order to deduce the differential equations determining ${\displaystyle u,v,w}$ we may arbitrarily use rectangular or polar coordinates; the latter however are here to be preferred. If differentiations