Newton, Isaac, Philosophia naturalis principia mathematica, 1713

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                  PROPOSITIO VIII. THEOREMA VIII.
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                  DE MUNDI
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                  SYSTEMATE</s>
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                  Si Globorum duorum in ſe mutuo gravitantium materia undique,
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                  in regionibus quæ à centris æqualiter diſtant, homogenea ſit:
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                  erit pondus Globi alterutrius in alterum reciproce ut quadra­
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                  tum diſtantiæ inter centra.
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                  <s>Poſtquam inveniſſem gravitatem in Planetam totum oriri &
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                  componi ex gravitatibus in partes; & eſſe in partes ſingulas reci­
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                  proce proportionalem quadratis diſtantiarum a partibus: dubita­
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                  bam an reciproca illa proportio duplicata obtineret accurate in vi
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                  tota ex viribus pluribus compoſita, an vero quam proxime. </s>
                  <s>Nam
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                  fieri poſſet ut proportio, quæ in majoribus diſtantiis ſatis accu­
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                  rate obtineret, prope ſuperficiem Planetæ ob inæquales particu­
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                  larum diſtantias & ſitus diſſimiles, notabiliter erraret. </s>
                  <s>Tandem
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                  vero, per Prop. LXXV. & LXXVI. Libri primi & ipſarum Corol­
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                  laria, intellexi veritatem Propoſitionis de qua hic agitur.
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                  Corol.
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                  1. Hinc inveniri & inter ſe comparari poſſunt pondera
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                  corporum in diverſos Planetas. </s>
                  <s>Nam pondera corporum æqua­
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                  lium circum Planetas in circulis revolventium ſunt (per Corol. 2.
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                  Prop. IV. Lib.I.) ut diametri circulorum directe & quadrata tem­
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                  porum periodieorum inverſe; & pondera ad ſuperficies Planeta­
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                  rum, aliaſve quaſvis a centro diſtantias, majora ſunt vel minora
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                  (per hanc Propoſitionem) in duplicata ratione diſtantiarum in­
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                  verſa. Sic ex temporibus periodicis Veneris circum Solem die­
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                  rum 224 & horarum 16 1/4, Satellitis extimi circumjovialis circum
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                  Jovem dierum 16 & horarum (16 1/15), Satellitis Hugeniani circum
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                  Saturnum dierum 15 & horarum 22 2/3, & Lunæ circum Terram
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                  dierum 27, hor. 7. min. 43, collatis cum diſtantia mediocri Vene­
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                  ris a Sole & cum elongationibus maximis heliocentricis Satellitis
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                  extimi circumjovialis a centro Jovis 8′. 21 1/2″, Satellitis Hugeniani
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                  a centro Saturni 3′. 20″, & Lunæ a Terra 10′, computum ineundo
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                  inveni quod corporum æqualium & a Sole, Jove, Saturno ac Terra
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                  æqualiter diſtantium pondera in Solem, Jovem, Saturnum ac Ter­
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                  ram forent ad invicem ut 1, (1/1033), (1/2411), & (1/227512) reſpective. </s>
                  <s>Eſt enim
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                  parallaxis Solis ex obſervationibus noviſſimis quaſi 10″, &
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                  Hal­
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                  leius
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                  noſter per emerſiones Jovis & Satellitum e parte obſcura
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                  </s>
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