If the reader has followed all our previous considerations, he will have no further difficulty in understanding the methods leading to the solution of the problem of gravitation.
We start off on a consideration of a Galileian domain1, i.e. a domain in which there is no gravitational field relative to the Galileian reference-body K. The behaviour of measuring-rods and clocks with reference to K is known from the special theory of relativity, likewise the behaviour of “isolated” material points; the latter move uniformly and in straight lines.
Now let us refer this domain to a random2 Gauss coordinate3 system or to a “mollusc” as reference-body K′. Then with respect to K′ there is a gravitational field G (of a particular kind). We learn the behavior of measuring-rods and clocks and also of freely-moving material points with reference to K′ simply by mathematical transformation4. We interpret this behaviour as the behaviour of measuring-rods, docks and material points tinder the influence of the gravitational field G. Hereupon we introduce a hypothesis: that the influence of the gravitational field on measuring-rods, clocks and freely-moving material points continues to take place according to the same laws, even in the case where the prevailing5 gravitational field is not derivable6 from the Galileian special care, simply by means of a transformation of co-ordinates.
The next step is to investigate the space-time behaviour of the gravitational field G, which was derived7 from the Galileian special case simply by transformation of the coordinates8. This behaviour is formulated9 in a law, which is always valid10, no matter how the reference-body (mollusc) used in the description may be chosen.
This law is not yet the general law of the gravitational field, since the gravitational field under consideration is of a special kind. In order to find out the general law-of-field of gravitation we still require to obtain a generalisation of the law as found above. This can be obtained without caprice, however, by taking into consideration the following demands:
(b) If there is any matter in the domain under consideration, only its inertial mass, and thus according to Section XV only its energy is of importance for its effect in exciting a field.
(c) Gravitational field and matter together must satisfy the law of the conservation of energy (and of impulse).
Finally, the general principle of relativity permits us to determine the influence of the gravitational field on the course of all those processes which take place according to known laws when a gravitational field is absent i.e. which have already been fitted into the frame of the special theory of relativity. In this connection we proceed in principle according to the method which has already been explained for measuring-rods, clocks and freely moving material points.
The theory of gravitation derived in this way from the general postulate of relativity excels not only in its beauty; nor in removing the defect attaching to classical mechanics which was brought to light in Section XXI; nor in interpreting the empirical law of the equality of inertial and gravitational mass; but it has also already explained a result of observation in astronomy, against which classical mechanics is powerless.
If we confine the application of the theory to the case where the gravitational fields can be regarded as being weak, and in which all masses move with respect to the coordinate system with velocities12 which are small compared with the velocity13 of light, we then obtain as a first approximation the Newtonian theory. Thus the latter theory is obtained here without any particular assumption, whereas Newton had to introduce the hypothesis that the force of attraction between mutually attracting material points is inversely14 proportional to the square of the distance between them. If we increase the accuracy of the calculation, deviations15 from the theory of Newton make their appearance, practically all of which must nevertheless escape the test of observation owing to their smallness.
We must draw attention here to one of these deviations. According to Newton’s theory, a planet moves round the sun in an ellipse, which would permanently16 maintain its position with respect to the fixed17 stars, if we could disregard the motion of the fixed stars themselves and the action of the other planets under consideration. Thus, if we correct the observed motion of the planets for these two influences, and if Newton’s theory be strictly18 correct, we ought to obtain for the orbit of the planet an ellipse, which is fixed with reference to the fixed stars. This deduction19, which can be tested with great accuracy, has been confirmed for all the planets save one, with the precision that is capable of being obtained by the delicacy20 of observation attainable21 at the present time. The sole exception is Mercury, the planet which lies nearest the sun. Since the time of Leverrier, it has been known that the ellipse corresponding to the orbit of Mercury, after it has been corrected for the influences mentioned above, is not stationary22 with respect to the fixed stars, but that it rotates exceedingly slowly in the plane of the orbit and in the sense of the orbital motion. The value obtained for this rotary23 movement of the orbital ellipse was 43 seconds of arc per century, an amount ensured to be correct to within a few seconds of arc. This effect can be explained by means of classical mechanics only on the assumption of hypotheses which have little probability, and which were devised solely24 for this purpose.
On the basis of the general theory of relativity, it is found that the ellipse of every planet round the sun must necessarily rotate in the manner indicated above; that for all the planets, with the exception of Mercury, this rotation25 is too small to be detected with the delicacy of observation possible at the present time; but that in the case of Mercury it must amount to 43 seconds of arc per century, a result which is strictly in agreement with observation.
Apart from this one, it has hitherto been possible to make only two deductions26 from the theory which admit of being tested by observation, to wit, the curvature of light rays by the gravitational field of the sun1, and a displacement27 of the spectral28 lines of light reaching us from large stars, as compared with the corresponding lines for light produced in an analogous29 manner terrestrially (i.e. by the same kind of atom)2. These two deductions from the theory have both been confirmed.
1 First observed by Eddington and others in 1919. (Cf. Appendix III, pp. 126–129). ↑
2 Established by Adams in 1924. (Cf. p. 132)
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1 domain | |
n.(活动等)领域,范围;领地,势力范围 | |
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2 random | |
adj.随机的;任意的;n.偶然的(或随便的)行动 | |
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3 coordinate | |
adj.同等的,协调的;n.同等者;vt.协作,协调 | |
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4 transformation | |
n.变化;改造;转变 | |
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5 prevailing | |
adj.盛行的;占优势的;主要的 | |
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6 derivable | |
adj.可引出的,可推论的,可诱导的 | |
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7 derived | |
vi.起源;由来;衍生;导出v.得到( derive的过去式和过去分词 );(从…中)得到获得;源于;(从…中)提取 | |
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8 coordinates | |
n.相配之衣物;坐标( coordinate的名词复数 );(颜色协调的)配套服装;[复数]女套服;同等重要的人(或物)v.使协调,使调和( coordinate的第三人称单数 );协调;协同;成为同等 | |
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9 formulated | |
v.构想出( formulate的过去式和过去分词 );规划;确切地阐述;用公式表示 | |
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10 valid | |
adj.有确实根据的;有效的;正当的,合法的 | |
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11 postulate | |
n.假定,基本条件;vt.要求,假定 | |
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12 velocities | |
n.速度( velocity的名词复数 );高速,快速 | |
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13 velocity | |
n.速度,速率 | |
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14 inversely | |
adj.相反的 | |
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15 deviations | |
背离,偏离( deviation的名词复数 ); 离经叛道的行为 | |
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16 permanently | |
adv.永恒地,永久地,固定不变地 | |
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17 fixed | |
adj.固定的,不变的,准备好的;(计算机)固定的 | |
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18 strictly | |
adv.严厉地,严格地;严密地 | |
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19 deduction | |
n.减除,扣除,减除额;推论,推理,演绎 | |
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20 delicacy | |
n.精致,细微,微妙,精良;美味,佳肴 | |
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21 attainable | |
a.可达到的,可获得的 | |
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22 stationary | |
adj.固定的,静止不动的 | |
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23 rotary | |
adj.(运动等)旋转的;轮转的;转动的 | |
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24 solely | |
adv.仅仅,唯一地 | |
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25 rotation | |
n.旋转;循环,轮流 | |
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26 deductions | |
扣除( deduction的名词复数 ); 结论; 扣除的量; 推演 | |
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27 displacement | |
n.移置,取代,位移,排水量 | |
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28 spectral | |
adj.幽灵的,鬼魂的 | |
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29 analogous | |
adj.相似的;类似的 | |
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