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Schwarzschild geodesics
In general relativity, the geodesics of the Schwarzschild metric describe the motion of particles of infinitesimal mass in the gravitational field of a central fixed mass ''M''. The Schwarzschild geodesics have been pivotal in the validation of the Einstein's theory of general relativity. For example, they provide quite accurate predictions of the anomalous precession of the planets in the Solar System, and of the deflection of light by gravity.
The Schwarzschild geodesics pertain only to the motion of particles of infinitesimal mass ''m'', i.e., particles that do not themselves contribute to the gravitational field. However, they are highly accurate provided that ''m'' is many-fold smaller than the central mass ''M'', e.g., for planets orbiting their sun. The Schwarzschild geodesics are also a good approximation to the relative motion of two bodies of arbitrary mass, provided that the Schwarzschild mass ''M'' is set equal to the sum of the two individual masses ''m''1 and ''m''2. This is important in predicting the motion of binary stars in general relativity.
==Historical context==
The Schwarzschild solution was found by Karl Schwarzschild shortly after Einstein published his field equations.
The Schwarzschild metric is named in honour of its discoverer Karl Schwarzschild, who found the solution in 1915, only about a month after the publication of Einstein's theory of general relativity. It was the first exact solution of the Einstein field equations other than the trivial flat space solution.
抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』
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