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A Lindblad resonance, named for the Swedish galactic astronomer Bertil Lindblad,〔, (Chapter 3, p. 149 ) 〕 is an orbital resonance in which an object's epicyclic frequency (the rate at which one periapse follows another) is a simple multiple of some forcing frequency. Resonances of this kind tend to increase the object's orbital eccentricity〔, (Page 162 ) 〕 and to cause its longitude of periapse to line up in phase with the forcing. Lindblad resonances drive spiral density waves〔, (Snippet page 73 ) 〕 both in galaxies (where stars are subject to forcing by the spiral arms themselves) and in Saturn's rings (where ring particles are subject to forcing by Saturn's moons). Lindblad resonances affect stars at such distances from a disc galaxy's centre where the natural frequency of the radial component of a star's orbital velocity is close to the frequency of the gravitational potential maxima encountered during its course through the spiral arms. If a star's orbital speed around the galactic centre is greater than that of the part of the spiral arm through which it is passing, then an inner Lindblad resonance occurs - if smaller, then an outer Lindblad resonance.〔, (Chapter 11, p. 147 ) 〕 At an inner resonance, a star's orbital speed is increased, moving the star outwards, and decreased for an outer resonance causing inward movement. ==References== *Murray, C.D., and S.F. Dermott 1999, ''Solar System Dynamics'' (Cambridge: Cambridge University Press). 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「Lindblad resonance」の詳細全文を読む スポンサード リンク
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