翻訳と辞書 Words near each other ・ "O" Is for Outlaw ・ "O"-Jung.Ban.Hap. ・ "Ode-to-Napoleon" hexachord ・ "Oh Yeah!" Live ・ "Our Contemporary" regional art exhibition (Leningrad, 1975) ・ "P" Is for Peril ・ "Pimpernel" Smith ・ "Polish death camp" controversy ・ "Pro knigi" ("About books") ・ "Prosopa" Greek Television Awards ・ "Pussy Cats" Starring the Walkmen ・ "Q" Is for Quarry ・ "R" Is for Ricochet ・ "R" The King (2016 film) ・ "Rags" Ragland ・ ! (album) ・ ! (disambiguation) ・ !! ・ !!! ・ !!! (album) ・ !!Destroy-Oh-Boy!! ・ !Action Pact! ・ !Arriba! La Pachanga ・ !Hero ・ !Hero (album) ・ !Kung language ・ !Oka Tokat ・ !PAUS3 ・ !T.O.O.H.! ・ !Women Art Revolution Dictionary Lists mini英和辞書 mini和英辞書 Webster 1913 Latin-English FOLDOC Wikipedia English ウィキペディア

翻訳と辞書　辞書検索 [ 開発暫定版 ] スポンサード リンク Lense-Thirring effect ： ウィキペディア英語版 Lense–Thirring precession In general relativity, Lense–Thirring precession or the Lense–Thirring effect (named after Josef Lense and Hans Thirring) is a relativistic correction to the precession of a gyroscope near a large rotating mass such as the Earth. It is a gravitomagnetic frame-dragging effect. According to a recent historical analysis by Pfister, the effect should be renamed as Einstein-Thirring-Lense effect. It is a prediction of general relativity consisting of secular precessions of the longitude of the ascending node and the argument of pericenter of a test particle freely orbiting a central spinning mass endowed with angular momentum $S$. The difference between de Sitter precession and the Lense–Thirring effect is that the de Sitter effect is due simply to the presence of a central mass, whereas the Lense–Thirring effect is due to the rotation of the central mass. The total precession is calculated by combining the de Sitter precession with the Lense–Thirring precession. ==Derivation== Before we can calculate this we want to find the gravitomagnetic field. The gravitomagnetic field in the equatorial plane of a rotating star: :$\backslash boldsymbol=\backslash fracR^q\backslash Big(\backslash boldsymbol\backslash cdot\backslash boldsymbol\backslash frac-\backslash frac\backslash frac\}\backslash Big).$ If we use then: :$\backslash boldsymbol=-4\backslash int\backslash frac.$ We get: :$\backslash boldsymbol=\backslash fracR^2\; q\backslash Big(\backslash boldsymbol\backslash cdot\backslash boldsymbol\backslash frac-\backslash frac\backslash frac$ \Big). When we look at Foucault's pendulum we only have to take the perpendicular-component to the Earth's surface. This means the first part of the equation cancels, where the radius $r$ equals $R$ and $\backslash theta$ is the latitude: :$\backslash boldsymbol\; =\; -\; \backslash left(\backslash frac\backslash frac$ \cos\theta\right). The absolute value of this would then be: :$\backslash boldsymbol=-\backslash frac\backslash frac$ \cos\theta. This is the gravitomagnetic field. We know there is a strong relation between the angular velocity in the local inertial system, $\backslash boldsymbol\_\; =\; -\backslash frac\backslash frac\backslash cos\backslash theta.$ As an example the latitude of the city of Nijmegen in the Netherlands is used for reference. This latitude gives a value for the Lense–Thirring precession of: :$\backslash Omega\_\backslash text=-2.2\; \backslash cdot\; 10^\; \backslash text/\backslash text.$ The total relativistic precessions on Earth is given by the sum of the De Sitter precession and the Lense–Thirring precession. This can be calculated by: :$\backslash Omega\_\backslash text\; =\; \backslash frac\; .$ At this rate a Foucault pendulum would have to oscillate for more than 16000 years to precess 1 degree. 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「Lense–Thirring precession」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.