Newton, Isaac
,
Philosophia naturalis principia mathematica
,
1713
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Eclipticæ;
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Q, q
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Quadraturas Lunæ in plano Eclipticæ, &
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p K
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perpendiculum in lineam
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Qq
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Quadraturis interjacentem. </
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<
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Solis ad perturbandum motum Lunæ (per Prop.xxv.) duplex eſt,
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altera lineæ
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LM,
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altera lineæ
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MT
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proportionalis. </
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<
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>Et Luna vi
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priore in Terram, poſteriore in Solem ſecundum lineam rectæ
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ST
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a Terra ad Solem ductæ parallelam trahitur. </
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LM
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agit ſecundum planum orbis Lunaris, & propterea ſitum plani nil
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mutat. </
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>Hæc igitur negligenda eſt. </
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MT
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qua planum
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Orbis Lunaris perturbatur eadem eſt cum vi 3
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PK
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vel 3
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IT.
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Et hæc vis (per Prop.xxv.) eſt ad vim qua Luna in circulo circa
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Terram quicſcentem tempore ſuo periodico uniformiter revolvi
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poſſet, ut 3
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IT
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ad Radium circuli multiplicatum per numerum
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178,725, ſive ut
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IT
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ad Radium multiplicatum per 59,575. Cæte
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rum in hoc calculo & eo omni qui ſequitur, conſidero lineas om
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nes a Luna ad Solem ductas tanquam parallelas lineæ quæ a Terra
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ad Solem ducitur, propterea quod inclinatio tantum fere minuit
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effectus omnes in aliquibus caſibus, quantum auget in aliis; &
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Nodorum motus mediocres quærimus, neglectis iſtiuſmodi minu
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tiis, quæ calculum nimis impeditum redderent. </
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