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(詳細はKepler's third law that, according to the weak-field and slow-motion approximation of general relativity, will be suffered by a particle in orbit around a (slowly) spinning body, such as a typical planet or star. ==Explanation== According to general relativity, in its weak-field and slow-motion linearized approximation, a slowly spinning body induces an additional component of the gravitational field that acts on a freely-falling test particle with a non-central, gravitomagnetic Lorentz-like force. Among its consequences on the particle's orbital motion there is a small correction to Kepler's third law, namely : where ''T''Kep is the particle's period, ''M'' is the mass of the central body, and ''a'' is the semimajor axis of the particle's ellipse. If the orbit of the particle is circular and lies in the equatorial plane of the central body, the correction is : where ''S'' is the central body's angular momentum and ''c'' is the speed of light in vacuum. Particles orbiting in opposite directions experience gravitomagnetic corrections ''T''Gvm with opposite signs, so that the difference of their orbital periods would cancel the standard Keplerian terms and would add the gravitomagnetic ones.〔 〕〔 〕〔 〕〔 〕〔 〕〔 〕〔 〕〔 〕〔 〕〔 〕〔 〕〔 〕 Note that the + sign occurs for particle's corotation with respect to the rotation of the central body, whereas the − sign is for counter-rotation. That is, if the satellite orbits in the same direction as the planet spins, it takes more time to make a full orbit, whereas if it moves oppositely with respect to the planet's rotation its orbital period gets shorter. 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「gravitomagnetic clock effect」の詳細全文を読む スポンサード リンク
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