Newton, Isaac, Philosophia naturalis principia mathematica, 1713

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                  Lunæ, determinavit quod elongatio maxima heliocentrica Satelli­
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                    <arrow.to.target n="note377"/>
                  tis extimi Jovialis a centro Jovis in mediocri Jovis a Sole diſtan­
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                  tia ſit 8′. 21 1/2″, & diameter Jovis 41″. Ex duratione Eclipſeon
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                  Satellitum in umbram Jovis incidentium prodit hæc diameter
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                  quaſi 40″, atque adeo ſemidiameter 20″. Menſuravit autem
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                  Hu­
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                  genius
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                  elongationem maximam heliocentricam Satellitis a ſe de­
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                  tecti 3′. 20″ a centro Saturni, & hujus elongationis pars quarta,
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                  nempe 50″, eſt diameter annuli Saturni e Sole viſi, & diameter Sa­
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                  turni eſt ad diametrum annuli ut 4 ad 9, ideoque ſemidiameter
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                  Saturni e Sole viſi eſt 11″. Subducatur lux erratica quæ haud
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                  minor eſſe ſolet quam 2″ vel 3″: Et manebit ſemidiameter Saturni
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                  quaſi 9″. Ex hiſce autem & Solis ſemidiametro mediocri 16′. 6″
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                  computum ineundo prodeunt veræ Solis, Jovis, Saturni ac Terræ
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                  ſemidiametri ad invicem ut 10000, 1077, 889 & 104. Unde,
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                  cum pondera æqualium corporum 2 centris Solis, Jovis, Saturni
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                  ac Terræ æqualiter diſtantium, ſint in Solem, Jovem, Saturnum
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                  ac Terram, ut 1, (1/1033), (1/2411), & (1/227512) reſpective, & auctis vel dimi­
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                  nutis diſtantiis pondera diminuantur vel augeantur in duplicata
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                  ratione: pondera æqualium corporum in Solem, Jovem, Satur­
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                  num ac Terram in diſtantiis 10000, 1077, 889, & 104 ab eorum
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                  centris, atque adeo in eorum ſuperficiebus, erunt ut 10000, 835,
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                  525, & 410 reſpective. </s>
                  <s>Quanta ſint pondera corporum in ſuper­
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                  ficie Lunæ dicemus in ſequentibus.
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                  LIBER
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                  TERTIUS.</s>
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                  Corol.
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                  2. Innoteſcit etiam quantitas materiæ in Planetis ſingulis.
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                  Nam quantitates materiæ in Planetis ſunt ut eorum vires in æqua­
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                  libus diſtantiis ab eorum centris, id eſt, in Sole, Jove, Saturno ac
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                  Terra ſunt ut 1, (1/1033), (1/2411), & (1/227512) reſpective. </s>
                  <s>Si parallaxis Solis
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                  ſtatuatur major vel minor quam 10″, debebit quantitas materiæ in
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                  Terra augeri vel diminui in triplicata ratione.
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                  </s>
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                <p type="main">
                  <s>
                    <emph type="italics"/>
                  Corol.
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                  3. Innoteſcunt etiam denſitates Planetarum. </s>
                  <s>Nam pon­
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                  dera corporum æqualium & homogeneorum in Sphæras homoge­
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                  neas ſunt in ſuperficiebus Sphærarum ut Sphærarum diametri, per
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                  Prop. LXXII. Lib. I. ideoque Sphærarum heterogenearum denſi­
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                  tates ſunt ut pondera illa applicata ad Sphærarum diametros.
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                  Erant autem veræ Solis, Jovis, Saturni ac Terræ diametri ad invi­
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                  cem ut 10000, 1077, 889, & 104, & pondera in eoſdem ut 10000,
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                  835, 525, & 410, & propterea denſitates ſunt ut 100, 78, 59,
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                  & 396. Denſitas Terræ quæ prodit ex hoc computo non pendet
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                  a parallaxi Solis, ſed determinatur per parallaxin Lunæ, & prop­
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                  </s>
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