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:''See also: Classical central-force problem'' In celestial mechanics, the specific relative angular momentum (h) of two orbiting bodies is the vector product of the relative position and the relative velocity. Equivalently, it is the total angular momentum divided by the reduced mass. Specific relative angular momentum plays a pivotal role in the analysis of the two-body problem. ==Definition== Specific relative angular momentum, represented by the symbol , is defined as the cross product of the relative position vector and the relative velocity vector . : where: * is the relative orbital position vector * is the relative orbital velocity vector * is the total angular momentum of the system (i.e. the sum of the angular momenta of each body) * is the reduced mass The units of are m2s−1. The vector is always perpendicular to the instantaneous osculating orbital plane, which coincides with the instantaneous perturbed orbit. It would not necessarily be perpendicular to an average plane which accounted for many years of perturbations. As usual in physics, the magnitude of the vector quantity is denoted by : : 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「specific relative angular momentum」の詳細全文を読む スポンサード リンク
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