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Einstein's Discovery of Gravitational Waves 1916-1918

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arxiv 1602.04040 v1 pith:XQAQEOEQ submitted 2016-02-12 physics.hist-ph

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keywords einsteinwavesgravitationalunimodularcoordinatescoordinaterestrictiveabove
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In his 1916 ground-breaking general relativity paper Einstein had imposed a restrictive coordinate condition, his field equations were valid for coordinate systems which are unimodular. Later, Einstein published a paper on gravitational waves. The solution presented in this paper did not satisfy the above restrictive condition. In his gravitational waves paper, Einstein concluded that gravitational fields propagate at the speed of light. The solution is the Minkowski flat metric plus a small disturbance propagating in a flat spacetime. Einstein calculated the small deviation from Minkowski metric in a manner analogous to that of retarded potentials in electrodynamics. However, in obtaining the above derivation, Einstein made a mathematical error. This error caused him to obtain three different types of waves compatible with his approximate field equations: longitudinal waves, transverse waves and a new type of wave. Einstein added an Addendum in which he suggested that in systems in unimodular coordinates only waves of the third type occur and these waves transport energy. He became obsessed with his unimodular coordinates. Einstein's colleagues demonstrated to him that in the coordinate system in unimodular coordinates the gravitational wave of a mass point carry no energy, but Einstein tried to persuade them that he had actually not made a mistake in his gravitational waves paper. Einstein, however, eventually accepted his colleagues results and dropped the restrictive unimodular coordinates. This finally led him to discover plane transverse gravitational waves.

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  1. Distinguishing scale-dependent Planck stars from renormalization group improved Schwarzschild black holes by Gravitational waves

    gr-qc 2025-06 conditional novelty 4.0 of 10

    Gravitational-wave strains from analytic-kludge EMRI models can distinguish scale-dependent Planck stars from renormalization-group improved Schwarzschild black holes, at least for the chosen orbit parameters.

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