Newton, Isaac, Philosophia naturalis principia mathematica, 1713

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                    <arrow.to.target n="note370"/>
                    <emph type="italics"/>
                  chonem
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                  56 1/2. Aſt
                    <emph type="italics"/>
                  Tycho,
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                  & quotquot ejus Tabulas refractionum
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                  ſequuntur, conſtituendo refractiones Solis & Lunæ (omnino con­
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                  tra naturam Lucis) majores quam Fixarum, idque ſcrupulis quaſi
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                  quatuor vel quinque, auxerunt parallaxin Lunæ ſcrupulis totidem,
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                  hoc eſt, quaſi duodecima vel decima quinta parte totius paralla­
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                  xeos. </s>
                  <s>Corrigatur iſte error, & diſtantia evadet quaſi 60 1/2 ſemi­
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                  diametrorum terreſtrium, fere ut ab aliis aſſignatum eſt. </s>
                  <s>Aſſuma­
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                  mus diſtantiam mediocrem ſexaginta ſemidiametrorum; & Luna­
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                  rem periodum reſpectu Fixarum compleri diebus 27, horis 7, mi­
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                  nutis primis 43, ut ab Aſtronomis ſtatuitur; atque ambitum Terræ
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                  eſſe pedum Pariſienſium 123249600, uti a
                    <emph type="italics"/>
                  Gallis
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                  menſurantibus de­
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                  finitum eſt: Et ſi Luna motu omni privari fingatur ac dimitti ut,
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                  urgente vi illa omni qua in Orbe ſuo retinetur, deſcendat in Ter­
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                  ram; hæc ſpatio minuti unius primi cadendo deſcribet pedes Pari­
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                  ſienſes (15 1/12). Colligitur hoc ex calculo vel per Propoſitionem
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                  XXXVI. Libri primi, vel (quod eodem recidit) per Corollarium
                    <lb/>
                  nonum Propoſitionis quartæ ejuſdem Libri, confecto. </s>
                  <s>Nam ar­
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                  cus illius quem Luna tempore minuti unius primi, medio ſuo
                    <lb/>
                  motu, ad diſtantiam ſexaginta ſemidiametrorum terreſtrium de­
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                  ſcribat, ſinus verſus eſt pedum Pariſienſium (15 1/12) circiter. </s>
                  <s>Unde
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                  cum vis illa accedendo ad Terram augeatur in duplicata diſtantiæ
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                  ratione inverſa, adeoque ad ſuperficiem Terræ major ſit partibus
                    <lb/>
                  60X60 quam ad Lunam; corpus vi illa in regionibus noſtris ca­
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                  dendo, deſcribere deberet ſpatio minuti unius primi pedes Pari­
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                  ſienſes 60X60X(15 1/12), & ſpatio minuti unius ſecundi pedes (15 1/12).
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                  Atqui corpora in regionibus noſtris vi gravitatis cadendo, deſcri­
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                  bunt tempore minuti unius ſecundi pedes Pariſienſes (15 1/12), uti
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                    <emph type="italics"/>
                  Hugenius
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                  factis pendulorum experimentis & computo inde inito,
                    <lb/>
                  demonſtravit: & propterea (per Reg. 1. & 11.) vis qua Luna in
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                  Orbe ſuo retinetur, illa ipſa eſt quam nos Gravitatem dicere ſole­
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                  mus. </s>
                  <s>Nam ſi Gravitas ab ea diverſa eſt, corpora viribus utriſque
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                  conjunctis Terram petendo, duplo velocius deſcendent, & ſpatio
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                  minuti unius ſecundi cadendo deſcribent pedes Pariſienſes 30 1/6:
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                  omnino contra Experientiam.
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                  </s>
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                <p type="margin">
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                    <margin.target id="note370"/>
                  DE MUNDI
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                  SYSTEMATE</s>
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                <p type="main">
                  <s>Calculus hic fundatur in hypotheſi quod Terra quieſcit. </s>
                  <s>Nam
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                  ſi Terra & Luna circum Solem moveantur, & interea quoque cir­
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                  cum commune gravitatis centrum revolvantur: diſtantia centro­
                    <lb/>
                  rum Lunæ ac Terræ ab invicem erit 60 1/2 ſemidiametrorum ter­
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                  reſtrium; uti computationem (per Prop. LX. Lib. I.) ineunti
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                  patebit.
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                  </s>
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