Galilei, Galileo
,
The systems of the world
,
1661
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inconcluſiveneſſe at leaſt of the demonſtrations of this Author,
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firſt propoſed to conſideration, and how both he, and all the
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Aſtronomers with whom he contendeth, do agree that the new
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Star had not any motion of its own, and onely went round with
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the diurnal motion of the
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primum mobile
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; but diſſent about the
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placing of it, the one party putting it in the Celeſtial Region,
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that is above the Moon, and haply above the fixed Stars, and
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the other judging it to be neer to the Earth, that is, under the
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concave of the Lunar Orb. </
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>And becauſe the ſituation of the new
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ſtar, of which we ſpeak, was towards the North, and at no very
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great diſtance from the Pole, ſo that to us
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Septentrionals,
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it did
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never ſet, it was an eaſie matter with Aſtronomical inſtruments
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to have taken its ſeveral meridian altitudes, as well its ſmalleſt
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under the Pole, as its greateſt above the ſame; from the
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ring of which altitudes, made in ſeveral places of the Earth,
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ſituate at different diſtances from the North, that is, different
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from one another in relation to polar altitudes, the ſtars diſtance
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might be inferred: For if it was in the Firmament amongſt the
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other fixed ſtars, its meridian altitudes taken in divers elevations
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of the pole, ought neceſſarily to differ from each other with the
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ſame variations that are found amongſt thoſe elevations
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ſelves; that is, for example, if the elevation of the ſtar above
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the horizon was 30 degrees, taken in the place where the polar
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altitude was
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v. </
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45 degrees, the elevation of the ſame ſtar
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ought to have been encreaſed 4 or 5 degrees in thoſe more
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thernly places where the pole was higher by the ſaid 4 or 5
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grees. </
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>But if the ſtars diſtance from the Earth was but very little,
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in compariſon of that of the Firmament; its meridian altitudes
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ought approaching to the North to encreaſe conſiderably more
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than the polar altitudes; and by that greater encreaſe, that is,
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by the exceſſe of the encreaſe of the ſtars elevation, above the
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encreaſe of the polar elevation (which is called the difference of
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Parallaxes) is readily calculated with a cleer and ſure method,
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the ſtars diſtance from the centre of the Earth. </
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>Now this Author
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taketh the obſervations made by thirteen Aſtronomers in ſundry
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elevations of the pole, and conferring a part of them at his
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ſure, he computeth by twelve collations the new ſtars height to
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have been alwayes beneath the Moon; but this he adventures to
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do in hopes to find ſo groſſe ignorance in all thoſe, into whoſe
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hands his book might come, that to ſpeak the truth, it hath turn'd
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my ſtomack; and I wait to ſee how thoſe other Aſtronomers, and
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particularly
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Kepler,
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againſt whom this Author principally
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veigheth, can contein themſelves in ſilence, for he doth not uſe
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to hold his tongue on ſuch occaſions; unleſſe he did poſſibly
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think the enterprize too much below him. </
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<
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>Now to give you to </
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