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翻訳と辞書　辞書検索 [ 開発暫定版 ] スポンサード リンク Longitude of the periapsis ： ウィキペディア英語版 Longitude of the periapsis In celestial mechanics, the longitude of the periapsis (symbolized ϖ) of an orbiting body is the longitude (measured from the point of the vernal equinox) at which the periapsis (closest approach to the central body) would occur if the body's inclination were zero. For motion of a planet around the Sun, this position could be called longitude of perihelion. The longitude of periapsis is a compound angle, with part of it being measured in the plane of reference and the rest being measured in the plane of the orbit. Likewise, any angle derived from the longitude of periapsis (e.g. mean longitude and true longitude) will also be compound. Sometimes, the term ''longitude of periapsis'' is used to refer to ω, the angle between the ascending node and the periapsis. That usage of the term is especially common in discussions of binary stars and exoplanets.〔See e.g. p. 201, (''The Binary Stars'' ), Robert Grant Aitken, Semicentennial Publications of the University of California, 1918, or (Format, ''Sixth Catalog of Orbits of Visual Binary Stars'' ), William I. Hartkopf & Brian D. Mason, U. S. Naval Observatory, Washington, D.C. Accessed on line October 25, 2008〕 However, the angle ω is less ambiguously known as the argument of periapsis. ==Calculation from state vectors== $\backslash varpi$ is the sum of the longitude of ascending node $\backslash Omega$ and the argument of periapsis $\backslash omega$: $\backslash varpi\; =\; \backslash Omega\; +\; \backslash omega$ which are derived from the orbital state vectors. 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「Longitude of the periapsis」の詳細全文を読む スポンサード リンク 翻訳と辞書 : 翻訳のためのインターネットリソース Copyright(C) kotoba.ne.jp 1997-2016. All Rights Reserved.