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Statements

Subject Item: dbr:List_of_contributors_to_general_relativity
dbo:wikiPageWikiLink: dbr:Mathisson–Papapetrou–Dixon_equations

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Subject Item: dbr:Mathisson-Papapetrou_equations
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Subject Item: dbr:Myron_Mathisson
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rdfs:label: Mathissonovy–Papapetrouovy–Dixonovy rovnice Mathisson–Papapetrou–Dixon equations
rdfs:comment: In physics, specifically general relativity, the Mathisson–Papapetrou–Dixon equations describe the motion of a massive spinning body moving in a gravitational field. Other equations with similar names and mathematical forms are the Mathisson–Papapetrou equations and Papapetrou–Dixon equations. All three sets of equations describe the same physics. They are named for M. Mathisson, W. G. Dixon, and A. Papapetrou. Throughout, this article uses the natural units c = G = 1, and tensor index notation. Ve fyzice, přesněji v obecné teorii relativity, soustava Mathissonových-Papapetrouových-Dixonových rovnic popisuje pohyb (klasické) testovací částice se dvěma vnitřními stupni volnosti -- hmotností (monopólem) a spinem (dipólem), ve vnějším gravitačním poli. Jsou odvozeny ze zákonů zachování a je pro ně charakteristické, že obecně algebraicky nespojují 4-hybnost a 4-rychlost spinující částice, což mimo jiné znamená, že 4-hybnost a 4-rychlost částice nemusejí být paralelní.
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dbo:abstract: In physics, specifically general relativity, the Mathisson–Papapetrou–Dixon equations describe the motion of a massive spinning body moving in a gravitational field. Other equations with similar names and mathematical forms are the Mathisson–Papapetrou equations and Papapetrou–Dixon equations. All three sets of equations describe the same physics. They are named for M. Mathisson, W. G. Dixon, and A. Papapetrou. Throughout, this article uses the natural units c = G = 1, and tensor index notation. Ve fyzice, přesněji v obecné teorii relativity, soustava Mathissonových-Papapetrouových-Dixonových rovnic popisuje pohyb (klasické) testovací částice se dvěma vnitřními stupni volnosti -- hmotností (monopólem) a spinem (dipólem), ve vnějším gravitačním poli. Jsou odvozeny ze zákonů zachování a je pro ně charakteristické, že obecně algebraicky nespojují 4-hybnost a 4-rychlost spinující částice, což mimo jiné znamená, že 4-hybnost a 4-rychlost částice nemusejí být paralelní.
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