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<v Speaker 1>Chapter sixteen, Part two of A Short Account of the

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<v Speaker 1>History of Mathematics. This is a LibriVox recording. All LibriVox

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<v Speaker 1>recordings are in the public domain. For more information or

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<v Speaker 1>to volunteer, please visit LibriVox dot org. This is a

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<v Speaker 1>reading by Paul King p J K dot scripts dot

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<v Speaker 1>MI I T dot E d U forward slash p

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<v Speaker 1>K J. A Short Account of the History of Mathematics

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<v Speaker 1>by W. W. Rowseball. Chapter sixteen, The Life and Works

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<v Speaker 1>of Newton, Part two, instigated by Halley. Newton now returned

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<v Speaker 1>to the problem of gravitation, and before the autumn of

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<v Speaker 1>sixteen eighty four he had worked out the substance of

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<v Speaker 1>propositions one through nineteen twenty one thirty thirty two through

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<v Speaker 1>thirty five in the first book of the Principia. These,

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<v Speaker 1>together with the notes on the laws of motion and

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<v Speaker 1>various lemmas, were read for his lectures in the Michailmas

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<v Speaker 1>Term sixteen eighty four. In November Halley received Newton's promised communication,

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<v Speaker 1>which probably consisted of the substance of propositions one eleven

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<v Speaker 1>and either seventeen or corollaries one of thirteen, and thereupon

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<v Speaker 1>he again went to Cambridge, where he saw a curious

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<v Speaker 1>treatise Desmo Too, drawn up since August. Most likely this

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<v Speaker 1>contained Newton's manuscript notes of the lectures above alluded to.

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<v Speaker 1>These notes are now in the University Library and are

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<v Speaker 1>headed de motu cooporum. Halley begged that the results might

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<v Speaker 1>be published, and finally secured a promise that they should

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<v Speaker 1>be sent to the Royal Society. They were accordingly communicated

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<v Speaker 1>to the Society not later than February sixteen eighty five,

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<v Speaker 1>in the paper desmo Too, which contained the substance of

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<v Speaker 1>the following propositions in the Principia Book I propositions one, four, six, seven, ten, eleven, fifteen,

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<v Speaker 1>seventeen thirty two and Book two Propositions two, three and four.

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<v Speaker 1>It seems also to have been due to the influence

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<v Speaker 1>in tact of Halley at this visit in November sixteen

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<v Speaker 1>eighty four, that Newton undertook to attack the whole problem

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<v Speaker 1>of gravitation and practically pledged himself to publish his results.

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<v Speaker 1>As yet, Newton had not determined the attraction of a

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<v Speaker 1>spherical body on an external point, nor had he calculated

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<v Speaker 1>the details of the planetary motions. Even if the members

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<v Speaker 1>of the Solar system could be regarded as points. The

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<v Speaker 1>first problem was solved in sixteen eighty five, probably either

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<v Speaker 1>in January or February. No sooner, to quote from doctor

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<v Speaker 1>Galicier's address on the Bison tenorary of the publication of

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<v Speaker 1>the Principia, had Newton proved the superb theorem. And we

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<v Speaker 1>know from his own words that he had no expectation

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<v Speaker 1>of so beautiful a result till it emerged from his

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<v Speaker 1>mathematical investigation that all the mechanism of the universe at

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<v Speaker 1>once lay spread before him. When he discovered the theorems

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<v Speaker 1>that from the first three sections of Book one, when

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<v Speaker 1>he gave them in his lectures of sixteen eighty four,

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<v Speaker 1>he was unaware that the Sun and Earth exerted their

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<v Speaker 1>attractions as if they were but points. How different must

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<v Speaker 1>these propositions have seen to Newton's eyes when he realized

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<v Speaker 1>that these results, which he had believed to be only

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<v Speaker 1>approximately true when applied to the Solar system, were really exact. Hitherto,

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<v Speaker 1>they had been only true in so far as he

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<v Speaker 1>could regard the Sun as a point compared to the

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<v Speaker 1>distance of the planets, or the Earth as a point

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<v Speaker 1>compared to the distance of the Moon, a distance amounting

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<v Speaker 1>to all about sixty times the Earth's radius. But now

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<v Speaker 1>they were mathematically true, excepting only for the slight deviation

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<v Speaker 1>from a perfectly spherical form of the Sun, Earth, and planets.

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<v Speaker 1>We can imagine the effect of this sudden transition from

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<v Speaker 1>approximation to exactitude in stimulating Newton's mind to still greater efforts.

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<v Speaker 1>It was now in his power to apply the mathematical

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<v Speaker 1>analysis with absolute precision to the actual problems of astronomy.

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<v Speaker 1>Of the three fundamental principles applied in the principia, we

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<v Speaker 1>may say that the idea that every particle attracts every

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<v Speaker 1>other particle in the universe was formed at least as

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<v Speaker 1>early as sixteen sixty six. The law of equable distribution

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<v Speaker 1>of areas its consequences, and the fact that if the

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<v Speaker 1>law of attraction were that of the inverse square of

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<v Speaker 1>the orbit of a particle about a center of force

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<v Speaker 1>would be a conic where proved in sixteen seventy nine.

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<v Speaker 1>And lastly, the discovery that a sphere whose density at

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<v Speaker 1>any point depends only on the distance from the center

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<v Speaker 1>attracts an external point as if the whole mass were

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<v Speaker 1>collected at its center were made in sixteen eighty five.

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<v Speaker 1>It was this last discovery that enabled him to apply

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<v Speaker 1>the first two principles to the phenomenon of bodies of

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<v Speaker 1>finite size. The draft of the first Book of the

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<v Speaker 1>Principia was finished before the summer of sixteen eighty five,

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<v Speaker 1>but the corrections and editions took some time, and the

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<v Speaker 1>book was not presented to the Royal Society until April

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<v Speaker 1>twenty eighth, sixteen eighty six. This book is given up

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<v Speaker 1>to the consideration of the motion of particles or bodies

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<v Speaker 1>in free space, either in known orbits, or under the

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<v Speaker 1>action of known forces, or under their mutual attraction. In it,

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<v Speaker 1>Uton generalizes the law of attraction into a statement that

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<v Speaker 1>every particle of matter in the universe attracts every other

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<v Speaker 1>particle with a force which varies directly as the product

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<v Speaker 1>of their masses and inversely as a square of the

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<v Speaker 1>distance between them, and he thence deduces the law of

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<v Speaker 1>attraction for spherical shells of constant density. The book is

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<v Speaker 1>prefaced by an introduction on the science of dynamics. The

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<v Speaker 1>second Book of the Principia was completed by the summer

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<v Speaker 1>of sixteen eighty six. This book treats of motion in

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<v Speaker 1>a resting medium, and of hydrostatics and hydrodynamics, with a

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<v Speaker 1>special application to waves, tides, and acoustics. He concludes it

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<v Speaker 1>by shewing that the Cartesian theory of vortices is inconsistent

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<v Speaker 1>both with the known facts and with the laws of motion.

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<v Speaker 1>The next nine or ten months were devoted to the

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<v Speaker 1>third book, probably for this he had originally no materials

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<v Speaker 1>ready in it. The theorems obtained in the first book

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<v Speaker 1>are applied to the chief phenomenon of the Solar System.

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<v Speaker 1>The masses and distances of the planets, and, wherever sufficient

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<v Speaker 1>data existed, of their satellites are determined. In particular, the

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<v Speaker 1>motion of the Moon, the various inequalities therein, and the

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<v Speaker 1>theory of the tides are worked out in detail. He

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<v Speaker 1>also investigates the theory of comets shoes that they belong

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<v Speaker 1>to the Solar system, explains how from three observations the

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<v Speaker 1>orbit can be determined, and illustrates his results by considering

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<v Speaker 1>certain special commets. The third book, as we have it,

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<v Speaker 1>is but little more than a sketch of what Newton

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<v Speaker 1>had finally proposed to himself to accomplish His original scheme

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<v Speaker 1>is among the Portsmouth papers and his notes shoe that

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<v Speaker 1>he continued to work at it for some years after

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<v Speaker 1>the publication of the first edition of the Principia. The

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<v Speaker 1>most interesting of his memoranda are those in which, by

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<v Speaker 1>means of fluxions, he has carried out his results beyond

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<v Speaker 1>the point at which he was able to translate them

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<v Speaker 1>into geometry footnote. I take this opportunity of saying that

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<v Speaker 1>I hope shortly to publish a memoir on the history

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<v Speaker 1>and compilation of the Principia. The following brief summary of

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<v Speaker 1>the contents of the work will give the reader a

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<v Speaker 1>general idea of its arrangement. The Principia is preceded by

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<v Speaker 1>a preface in which Newton says that his object is

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<v Speaker 1>to apply mathematics to the phenomena of nature. Among these phenomena,

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<v Speaker 1>motion is one of the most important. Now, motion is

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<v Speaker 1>the effective force, and though he does not know what

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<v Speaker 1>is the nature or origin of force, still many of

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<v Speaker 1>its effects can be measured, and it is these that

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<v Speaker 1>form the subject matter of the work. The work begins, therefore, naturally,

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<v Speaker 1>with an introduction on dynamics, the science of motion, This

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<v Speaker 1>commences with the eight definitions of the various terms such

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<v Speaker 1>as mass, momentum, and so on. Newton then lays down

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<v Speaker 1>three laws of motion, which are incapable of exact proof,

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<v Speaker 1>but are confirmed partly by direct experiments, partly by the

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<v Speaker 1>agreement with observation of the deductions from them. From these

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<v Speaker 1>he deduces six fundamental principles of mechanics and adds an

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<v Speaker 1>appendix on the motion of falling bodies, projectiles, oscillations, impact,

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<v Speaker 1>and the mutual attractions of two bodies. The most important

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<v Speaker 1>deduction is that of the parallelogram of velocities, accelerations, and forces.

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<v Speaker 1>The first book of the Principia is on the motion

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<v Speaker 1>of bodies in free space, and is divided into fourteen sections.

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<v Speaker 1>The first section consists of eleven preliminary lemmas treated by

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<v Speaker 1>the method of prime and ultimate ratios and not by

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<v Speaker 1>that of indivisibles. The second section commences by shewing that

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<v Speaker 1>if a body such as a planet, revolve in an

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<v Speaker 1>orbit subject to a force tending to affix points such

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<v Speaker 1>as the Sun, the areas swept out by radii drawn

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<v Speaker 1>from the body to the point are in one plane

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<v Speaker 1>and are proportional to the times of describing them, and conversely,

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<v Speaker 1>if the areas be proportional to the times, the force

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<v Speaker 1>acting on the body must be directed to the point.

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<v Speaker 1>Newton then chows how if the orbit be known and

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<v Speaker 1>the center of force be given, the law of force

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<v Speaker 1>can be determined, and he finds the law for various curves.

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<v Speaker 1>In the third section, he applies these propositions to a

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<v Speaker 1>body which describes a conic section about a focus, and

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<v Speaker 1>proves that the force must vary inversely as a square

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<v Speaker 1>of the distance, and that Kepler's third law would necessarily

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<v Speaker 1>be true of such a system. He proves that if

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<v Speaker 1>a body were projected in any way and subject to

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<v Speaker 1>a central force which varied according to this law, then

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<v Speaker 1>it must move in a conic section having the center

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<v Speaker 1>of force in a focus. He concludes proposition seventeen corollaries

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<v Speaker 1>three and four with a suggestion as to how the

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<v Speaker 1>effects of distributing forces should be calculated. This was first

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<v Speaker 1>done by the brilliant investigations of Laplace and Lagrange, and

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<v Speaker 1>Laplace says that Lagrange's paper in the Berlin Memoirs for

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<v Speaker 1>seventeen eighty six, on which the modern treatment of the

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<v Speaker 1>subject is founded, was suggested by these remarks of Newton.

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<v Speaker 1>The fourth and fifth sections are devoted to the geometry

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<v Speaker 1>of conic sections, especially to the construction of conics, which

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<v Speaker 1>satisfy five conditions. In section four. One of the conditions

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<v Speaker 1>is that the focus is given. This includes the problem

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<v Speaker 1>of finding the path of a comet from three observations,

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<v Speaker 1>with which Newton says he found the most difficult problem

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<v Speaker 1>of any which he had to solve curiously enough. He

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<v Speaker 1>gave a second solution of the problem in Book three,

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<v Speaker 1>proposition forty one, in which he recommended as more simple,

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<v Speaker 1>but which is inapplicable in practice. The sixth section is

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<v Speaker 1>devoted to determining what at any given time is the

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<v Speaker 1>velocity and what is the position of a body, which

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<v Speaker 1>is describing a given conic about a center of attraction

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<v Speaker 1>in a focus, together with various converse problems. To effect this,

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<v Speaker 1>Newton had to find the area of a sector of

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<v Speaker 1>a conic. This is easily done for the parabola. He

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<v Speaker 1>then endeavors to shew that the exact quadrature of any

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<v Speaker 1>closed oval curve having no infinite branches, such as the ellipse,

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<v Speaker 1>is impossible. The proof is not correct, as it stands

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<v Speaker 1>since the result is not true for ovals of the

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<v Speaker 1>form why to the power of two M equals the

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<v Speaker 1>quantity A to the power of t two n minus

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<v Speaker 1>x to the power of two n all multiplied by

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<v Speaker 1>two to the power of two m times n to

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<v Speaker 1>the power of two m multiplied by x to the

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<v Speaker 1>power of two M times two n minus one, where

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<v Speaker 1>M and n are positive integers. Newton seems himself to

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<v Speaker 1>have felt some doubt about inserting it, though he believed

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<v Speaker 1>the result to be true, an exact quadrature being impossible.

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<v Speaker 1>He proceeds to give three ways, two arithmetical and one geometrical,

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<v Speaker 1>of approximating to the sectorial area of an ellipse as

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<v Speaker 1>closely as is desired. The seventh section is given up

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<v Speaker 1>to the discussion of motion in a straight line under

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<v Speaker 1>a force which varies inversely as a square of the

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<v Speaker 1>distance and its comparison with the motion, and a conic

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<v Speaker 1>under the same force. He concludes by giving a general

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<v Speaker 1>solution for all the problems considered in this section. For

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<v Speaker 1>X any law of force. He here determines geometrically, what

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<v Speaker 1>is equivalent of finding the integral of X divided by

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<v Speaker 1>the square root of the quantity ax minus x squared.

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<v Speaker 1>The eighth section contains a general solutions for any orbit

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<v Speaker 1>described under any central force of some of the problems

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<v Speaker 1>previously considered. In proposition forty he states that the kinetic

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<v Speaker 1>energy acquired by a body and moving from one point

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<v Speaker 1>to another is equal to the total work done by

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<v Speaker 1>the force between those two points. In the ninth section,

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<v Speaker 1>he discusses the case or the orbit is in motion

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<v Speaker 1>in its own plane round the center of force, and

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<v Speaker 1>treats in detail of the motion of the apse line

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<v Speaker 1>and the forces by which a given motion would be produced.

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<v Speaker 1>Newton applied this reasoning proposition forty five corollary IWO to

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<v Speaker 1>the case of the moon, but the resulting motion of

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<v Speaker 1>the apses only came out about one half of the

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<v Speaker 1>actual amount. The approximation was, in fact not carried to

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<v Speaker 1>a sufficiently high order. Newton was aware of the discrepancy,

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<v Speaker 1>and as he explained the similar difficulty in the case

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<v Speaker 1>of the nodes, it had been long suspected Goldfrays Lunar Theory,

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<v Speaker 1>second Edition, Article sixty eight that this scolium of the

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<v Speaker 1>first edition to book three, Proposition thirty five meant that

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<v Speaker 1>he had found the explanation. Nowhere in the principia does he, however,

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<v Speaker 1>give any hint as to how this was affected, and

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<v Speaker 1>that the true explanation of a difference which had long

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<v Speaker 1>formed an obstacle to the universal acceptance of the Newtonian system,

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<v Speaker 1>was first given by claireaut in seventeen fifty two. The

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<v Speaker 1>Portsmouth Papers contained Newton's original work, and shew that he

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<v Speaker 1>had obtained the true value by carrying the approximation to

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<v Speaker 1>a sufficiently high order. It also seemed clear from these

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<v Speaker 1>papers that Newton gave the corollary to Book one proposition

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<v Speaker 1>forty five as a mere illustration to the motion of

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<v Speaker 1>the apses and orbits, which are nearly circular, and did

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<v Speaker 1>not mean it to apply to the moon. But by

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<v Speaker 1>an inadvertence in the second and third editions, a reference

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<v Speaker 1>to it as an authenticity for a result connected with

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00:16:21.919 --> 00:16:25.840
<v Speaker 1>the moon was added, which would naturally deceive any reader.

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<v Speaker 1>Newton left most of the revision to the second edition

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<v Speaker 1>to Cotes, and it is probable that the mistake is

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<v Speaker 1>due to a blunder of the editor. Other questions connected

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<v Speaker 1>with lunar and planetary irregularities are also discussed in this proposition,

249
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<v Speaker 1>but the extreme conclusions of Newton misled all the early

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<v Speaker 1>commentators and even Laplace in his se stem de Monde,

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<v Speaker 1>published in seventeen ninety six, speaks of Newton as having

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<v Speaker 1>only roughly sketched out this part of the subject, leaving

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<v Speaker 1>it to be completed when the calculus should be further perfected.

254
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<v Speaker 1>But in the last volume of his Mechanique Cerest, published

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<v Speaker 1>in eighteen twenty five, he says that on more careful reading,

256
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<v Speaker 1>he has no hesitation in regarding it as among the

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<v Speaker 1>most profound parts of the work. The tenth section is

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<v Speaker 1>devoted to the consideration of motion of bodies along given surfaces,

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00:17:24.839 --> 00:17:27.599
<v Speaker 1>but not in planes passing through the center of force,

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<v Speaker 1>with special reference to the vibration of pendulums and the

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00:17:32.119 --> 00:17:36.720
<v Speaker 1>determination of the accelerating effect of gravity. In connection with

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<v Speaker 1>the latter problem, Newton investigates the chief geometrical properties of cycloids, epicycloids,

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<v Speaker 1>and hypocycloids. In the eleventh section are considered the problems

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<v Speaker 1>connected with motions in orbits where the center of forces

265
00:17:52.279 --> 00:17:56.319
<v Speaker 1>disturbed or the moving body is disturbed by other forces.

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<v Speaker 1>Until calculus of variations was invented by lug in seventeen

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<v Speaker 1>fifty five, it was impossible to do more than sketch

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<v Speaker 1>out the principles on which the problem should be solved,

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<v Speaker 1>and laplace in his mechanique. Cerest was the first to

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<v Speaker 1>work out most of the questions in any detail. Newton

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<v Speaker 1>commences by considering the disturbance produced by the mutual action

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<v Speaker 1>of two bodies revolving around one another. He then proceeds

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<v Speaker 1>to consider the problem of three or more bodies which

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<v Speaker 1>mutually attract one another. He first solves the question completely

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<v Speaker 1>if the force of attraction varies directly as the distance.

276
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<v Speaker 1>He next takes the case of the three bodies moving

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<v Speaker 1>under their mutual attractions as in nature. This problem has

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<v Speaker 1>not been yet solved generally, but in Newton's day it

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00:18:46.079 --> 00:18:48.920
<v Speaker 1>was beyond any analysis of which he had the command.

280
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<v Speaker 1>He contrived, however, to work out roughly the chief effects

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<v Speaker 1>of the disturbing action of the Sun on the motion

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<v Speaker 1>of the moon proposition sixty six. Position was singled out

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<v Speaker 1>by Lagrange as the most striking single illustration of the

284
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<v Speaker 1>genius of Newton. To this proposition, twenty two corollaries are appended,

285
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<v Speaker 1>in which it is applied to determine the motion in longitude.

286
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<v Speaker 1>In latitude, the annual equation, the motion of the apse

287
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<v Speaker 1>line and of the nodes, the evection, the change and

288
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<v Speaker 1>inclination of the plane of the lunar orbit, the precession

289
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<v Speaker 1>of the equinoxes, and the theory of the tides. The

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00:19:28.599 --> 00:19:31.519
<v Speaker 1>greater part of the third book consists of the numerical

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<v Speaker 1>application of these principles to the case of the moon

292
00:19:34.880 --> 00:19:38.519
<v Speaker 1>in the Earth. Lastly, Newton showed how from the motion

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<v Speaker 1>of the nodes of the interior, constitution of the body

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00:19:42.400 --> 00:19:46.160
<v Speaker 1>could be roughly determined. Up to this point, Newton had

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<v Speaker 1>generally treated the bodies with which he dealt as if

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00:19:49.640 --> 00:19:53.160
<v Speaker 1>they were particles. He now proceeds in section twelve to

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<v Speaker 1>consider the attraction of spherical masses, which are either of

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<v Speaker 1>uniform density or whose density at an point is a

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<v Speaker 1>single valued function of the distance of the point from

300
00:20:04.079 --> 00:20:06.960
<v Speaker 1>the center of the sphere. These are worked out for

301
00:20:07.039 --> 00:20:11.880
<v Speaker 1>any law of attraction. In section thirteen he gives some

302
00:20:12.039 --> 00:20:15.440
<v Speaker 1>general theorems on the theory of attractions and on some

303
00:20:15.720 --> 00:20:20.160
<v Speaker 1>propositions dealing with the attractions of solids of revolution. But

304
00:20:20.240 --> 00:20:23.759
<v Speaker 1>these problems are almost insoluble without the aid of the

305
00:20:23.799 --> 00:20:29.640
<v Speaker 1>infinitesimal calculus and the Newtonian account of them is incomplete.

306
00:20:31.559 --> 00:20:34.960
<v Speaker 1>The fourteenth section contains a statement of some theories and

307
00:20:35.079 --> 00:20:39.240
<v Speaker 1>experiments in physical optics, and a solution by geometry of

308
00:20:39.319 --> 00:20:42.759
<v Speaker 1>some problems in geometrical optics, particularly on the form of

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<v Speaker 1>aplanatic refracting surfaces of revolution. The second book of the

310
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<v Speaker 1>Principia is concerned with hydromechanics, and especially with motion in

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<v Speaker 1>a resisting medium. These questions are not worked out so

312
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<v Speaker 1>completely as those treated in the first book, and though

313
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<v Speaker 1>this book provided the basis on which much of the

314
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<v Speaker 1>subsequent work of Danielle Bernoulli, clairout De, Lambert, Euler and

315
00:21:09.559 --> 00:21:13.519
<v Speaker 1>Laplace were erected, it is not of the same epoch

316
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<v Speaker 1>making character as the first book. This book is divided

317
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<v Speaker 1>into nine sections. The motion of bodies in a medium

318
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<v Speaker 1>where the resistance varies directly as the velocity is considered

319
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<v Speaker 1>in the first section. The motions where resistance varies as

320
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<v Speaker 1>the square of the velocity is discussed in the second section.

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<v Speaker 1>The motion where the resistance can be expressed as a

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<v Speaker 1>sum of two terms, one of which varies as the velocity,

323
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<v Speaker 1>and the others the square of the velocity, is dealt

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<v Speaker 1>with in the third section. The second section contains proposition

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<v Speaker 1>twenty five, a construction for the shape of the solid

326
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<v Speaker 1>of least resistance. No proof is given, and it had

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<v Speaker 1>been long somewhat of a mystery to know how Newton

328
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<v Speaker 1>had contrived to solve the problem without the use of

329
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<v Speaker 1>calculus of variations. Newton's demonstrations, there are two of them,

330
00:22:08.559 --> 00:22:13.359
<v Speaker 1>have been recently discovered in the Portsmouth collection. The fourth

331
00:22:13.440 --> 00:22:17.680
<v Speaker 1>section is devoted to a spiral motion in a resisting medium,

332
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<v Speaker 1>the fifth to the theory of hydrostatics and elastic fluids,

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<v Speaker 1>the sixth to the motion of pendulums in a resisting medium,

334
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<v Speaker 1>the seventh to hydrodynamics, especially to the motion of projectiles

335
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<v Speaker 1>in air and other fluids. The eighth to the theory

336
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<v Speaker 1>of waves, including the principles from which the chief effects

337
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<v Speaker 1>of the wave hypotheses in light and sound are calculated,

338
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<v Speaker 1>and in particular the velocity of sound is determined. In

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<v Speaker 1>a ninth section, Newton discusses the Cartesian theory of vortices.

340
00:22:55.119 --> 00:22:58.400
<v Speaker 1>He begins by shewing that if there were no internal friction,

341
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<v Speaker 1>the motion would be impossible. He must therefore assume some

342
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<v Speaker 1>law of friction, and as a working hypothesis he supposes

343
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<v Speaker 1>that the resistance arising from want of lubricity in the

344
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<v Speaker 1>parts of a fluid is catius peribus proportional to the

345
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<v Speaker 1>velocity of which the parts of the fluid are separated

346
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<v Speaker 1>from each other. This hypothesis, as he himself remarks, is

347
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<v Speaker 1>probably not altogether correct, but he thinks that it will

348
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<v Speaker 1>give a general idea of the motion. He next proves

349
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<v Speaker 1>that on this hypothesis that the motion would be unstable.

350
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<v Speaker 1>He must therefore suppose that some constraining force prevents this catastrophe,

351
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<v Speaker 1>and he then chows that in that case, Kepler's third

352
00:23:44.359 --> 00:23:47.880
<v Speaker 1>law could not be true. Lastly, he chows, by independent

353
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<v Speaker 1>reasoning that the hypothesis must lead to results which are

354
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<v Speaker 1>inconsistent with Kepler's other two laws, and that both the

355
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<v Speaker 1>vortices and the motion of the planets would necessarily be unstable.

356
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<v Speaker 1>Several continental mathematicians made attempts to modify the Cartesian hypothesis

357
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<v Speaker 1>so as to avoid these conclusions, but they could never

358
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<v Speaker 1>explain one phenomenon without introducing fresh difficulties. It may be

359
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<v Speaker 1>taken that by seventeen fifty the Cartesian theory was finally abandoned.

360
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<v Speaker 1>The third book is headed on the system of the world,

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<v Speaker 1>and is concerned chiefly with the application of the results

362
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<v Speaker 1>of the first book to the Solar System. It is

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<v Speaker 1>introduced by certain rules of philosophizing and as a list

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<v Speaker 1>of certain data obtained from astronomical observations. The rules are one,

365
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<v Speaker 1>we may only assume as the possible causes of phenomenon,

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<v Speaker 1>such causes as are sufficient to explain them, and are

367
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<v Speaker 1>also verai kausi, a vera causa being one which is

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<v Speaker 1>capable of detection and such that its connection with the

369
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<v Speaker 1>phenomenon can be ultimate shewn by independent evidence. Two effects

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<v Speaker 1>of a similar kind must have similar causes. Three, whatever

371
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<v Speaker 1>properties of bodies are found by experience to be invariable

372
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<v Speaker 1>should be assumed to be so in places where direct

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<v Speaker 1>experiments cannot be made. Newton commences by illustrating the universality

374
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<v Speaker 1>of the law of gravitation and sketches out the principles

375
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<v Speaker 1>which lead him to think that the Solar system is

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<v Speaker 1>necessarily stable. He determines that the mass of the Moon,

377
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<v Speaker 1>the masses of the planets, their distances from the Sun,

378
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<v Speaker 1>and their figures. In the first edition, he estimated proposition

379
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<v Speaker 1>thirty seven that the ratio of the mass of the

380
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<v Speaker 1>Moon to that of the Earth was approximately that of

381
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<v Speaker 1>one to twenty six. In the second and third editions

382
00:25:48.960 --> 00:25:51.400
<v Speaker 1>this was altered to a ratio which is nearly that

383
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<v Speaker 1>of one in forty. But except for the mass of

384
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<v Speaker 1>the moon, he approximates to the results now known with

385
00:25:57.720 --> 00:26:02.319
<v Speaker 1>astonishing closeness. He finds the disturbing force exerted by the

386
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<v Speaker 1>Sun and the Moon, and considers the five chief irregularities

387
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<v Speaker 1>in the orbit of the Moon. He next discusses the

388
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<v Speaker 1>solar and lunar tides, determines the precession of the equinoxes,

389
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<v Speaker 1>and finally shows how the elements of a comet can

390
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<v Speaker 1>be determined by these observations, and applies his results to

391
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<v Speaker 1>certain comets. Before this time it had been commonly believed

392
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<v Speaker 1>that the comets had nothing to do with the Solar system,

393
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<v Speaker 1>though in sixteen eighty one d'orfel had shewn that the

394
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<v Speaker 1>path of the Great Comet of sixteen eighty was a

395
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<v Speaker 1>parabola having the Sun at its focus. Lastly, the precipia

396
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<v Speaker 1>is concluded by a general scolium containing the reflection on

397
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<v Speaker 1>the constitution of the universe and on the eternal, the

398
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<v Speaker 1>infinite and perfect being by whom it is governed. The

399
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<v Speaker 1>chief alterations in the second edition, published in seventeen thirteen

400
00:27:00.559 --> 00:27:03.960
<v Speaker 1>were the substitutions of simpler proofs for some of the

401
00:27:04.000 --> 00:27:07.599
<v Speaker 1>propositions in the second edition of the first book, a

402
00:27:07.599 --> 00:27:11.880
<v Speaker 1>more full and accurate investigation found on some fresh experiments

403
00:27:11.920 --> 00:27:15.400
<v Speaker 1>made by Newton about the year sixteen ninety and the

404
00:27:15.440 --> 00:27:18.799
<v Speaker 1>resistance of fluids in the seventh section of the second book,

405
00:27:19.319 --> 00:27:22.680
<v Speaker 1>and the addition of a detailed examination of the causes

406
00:27:23.039 --> 00:27:26.839
<v Speaker 1>of the precession of the equinoxes and the theory of

407
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<v Speaker 1>comets in the third book. The chief alterations in the

408
00:27:30.960 --> 00:27:34.359
<v Speaker 1>third edition, published in seventeen twenty six were in the

409
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<v Speaker 1>Scholium of Inflections and the edition of a new Scolium

410
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<v Speaker 1>on the Motion of the Moon's nodes, Book three, Proposition

411
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<v Speaker 1>fifty three, end of footnote. The demonstrations throughout the work

412
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<v Speaker 1>are geometrical, but to readers of ordinary ability are rendered

413
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<v Speaker 1>unnecessarily difficult by the absence of illustrations and explanations, by

414
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<v Speaker 1>the fact that no clue is given to the method

415
00:28:03.279 --> 00:28:07.119
<v Speaker 1>by which Newton arrived at his results. The reason why

416
00:28:07.160 --> 00:28:10.200
<v Speaker 1>it was presented in a geometrical form appears to have

417
00:28:10.240 --> 00:28:15.119
<v Speaker 1>been that the infinitetesimal calculus was then unknown, and had

418
00:28:15.160 --> 00:28:17.799
<v Speaker 1>Newton used it to determine the results, which were in

419
00:28:17.880 --> 00:28:21.440
<v Speaker 1>themselves opposed to the prevalent philosophy of the time, the

420
00:28:21.519 --> 00:28:24.680
<v Speaker 1>controversy as to the truth of his results would have

421
00:28:24.720 --> 00:28:28.079
<v Speaker 1>been hampered by a dispute concerning the validity of the

422
00:28:28.119 --> 00:28:32.119
<v Speaker 1>methods used in proving them. He therefore cast the whole

423
00:28:32.200 --> 00:28:37.119
<v Speaker 1>reasoning into a geometrical shape, which, if somewhat longer, can

424
00:28:37.160 --> 00:28:41.759
<v Speaker 1>at any rate be made intelligible to all mathematical students.

425
00:28:42.440 --> 00:28:45.359
<v Speaker 1>So closely did he follow the lines of Greek geometry

426
00:28:45.839 --> 00:28:51.359
<v Speaker 1>that he constantly used graphical methods and represented forces, velocities,

427
00:28:51.400 --> 00:28:55.880
<v Speaker 1>and other magnitude in the Euclidean way by straight lines

428
00:28:56.839 --> 00:29:01.279
<v Speaker 1>Book one lemma En, and not by certain number of units.

429
00:29:02.160 --> 00:29:05.720
<v Speaker 1>The latter and modern method had been introduced by Wallace

430
00:29:05.960 --> 00:29:09.039
<v Speaker 1>and must have been familiar to Newton. The effect of

431
00:29:09.079 --> 00:29:12.960
<v Speaker 1>his confining himself rigorously to classical geometry is that the

432
00:29:12.960 --> 00:29:16.680
<v Speaker 1>Principia is written in a language which is archaic, even

433
00:29:16.720 --> 00:29:20.680
<v Speaker 1>if not unfamiliar. The adoption of geometrical methods in the

434
00:29:20.680 --> 00:29:25.240
<v Speaker 1>Principia for purposes of demonstration does not indicate a preference

435
00:29:25.319 --> 00:29:29.319
<v Speaker 1>on Newton's part for geometry over analysis as an instrument

436
00:29:29.359 --> 00:29:32.880
<v Speaker 1>of research. For it is known now that Newton used

437
00:29:32.880 --> 00:29:36.400
<v Speaker 1>the fluctional calculus in the first instance in finding some

438
00:29:36.480 --> 00:29:40.240
<v Speaker 1>of the theorems, especially those towards the end of Book one

439
00:29:40.799 --> 00:29:42.680
<v Speaker 1>and in Book two, And in fact one of the

440
00:29:42.680 --> 00:29:46.160
<v Speaker 1>most important uses of that calculus is stated in Book

441
00:29:46.200 --> 00:29:49.200
<v Speaker 1>two Lemma I. But it is only just to remark

442
00:29:49.279 --> 00:29:51.799
<v Speaker 1>that at the time of its publication, and for nearly

443
00:29:51.880 --> 00:29:56.359
<v Speaker 1>a century afterwards, the differential and fluctional calculus were not

444
00:29:56.400 --> 00:29:59.920
<v Speaker 1>fully developed and did not possess the same superiority or

445
00:30:00.000 --> 00:30:02.519
<v Speaker 1>over the method he adopted by which they do now.

446
00:30:03.519 --> 00:30:06.279
<v Speaker 1>And it is a matter of astonishment that when Newton

447
00:30:06.400 --> 00:30:09.599
<v Speaker 1>did employ the calculus, he was able to use it

448
00:30:09.680 --> 00:30:12.839
<v Speaker 1>to so good an effect. The ability shewn in the

449
00:30:12.880 --> 00:30:16.720
<v Speaker 1>translation in a few months of theorems so numerous and

450
00:30:16.839 --> 00:30:20.079
<v Speaker 1>of so great complexity into the language of the geometry

451
00:30:20.079 --> 00:30:24.519
<v Speaker 1>of our Chimytes and Apollonius is I suppose unparalleled in

452
00:30:24.559 --> 00:30:29.880
<v Speaker 1>the history of mathematics. The printing of the work was slow,

453
00:30:30.440 --> 00:30:32.799
<v Speaker 1>and it was not finally published till the summer of

454
00:30:32.839 --> 00:30:38.279
<v Speaker 1>sixteen eighty seven. The whole cost was borne by Halle,

455
00:30:38.279 --> 00:30:40.759
<v Speaker 1>who also corrected the proofs and even put his own

456
00:30:40.799 --> 00:30:45.279
<v Speaker 1>researches on one side to press the printing forward. The conciseness,

457
00:30:45.559 --> 00:30:50.079
<v Speaker 1>absence of illustrations, and synthetical character of the book restricted

458
00:30:50.079 --> 00:30:53.799
<v Speaker 1>the numbers of those who were able to appreciate its value,

459
00:30:54.559 --> 00:30:58.400
<v Speaker 1>And though nearly all competent critics admitted the validity of

460
00:30:58.480 --> 00:31:02.400
<v Speaker 1>the conclusions, so little time elapse before it affected the

461
00:31:02.440 --> 00:31:06.559
<v Speaker 1>current beliefs of educated men. I should be inclined to say,

462
00:31:06.759 --> 00:31:10.799
<v Speaker 1>but on this point opinions differ widely that within ten

463
00:31:10.920 --> 00:31:14.039
<v Speaker 1>years of its publication it was generally accepted in Britain

464
00:31:14.160 --> 00:31:16.799
<v Speaker 1>as giving a correct account of the laws of the universe.

465
00:31:17.519 --> 00:31:21.119
<v Speaker 1>It was similarly accepted within about twenty years on the continent,

466
00:31:21.240 --> 00:31:24.880
<v Speaker 1>except in France, where the Cartesian hypothesis held its ground

467
00:31:24.960 --> 00:31:28.440
<v Speaker 1>until Voltaire in seventeen thirty eight took up the advocacy

468
00:31:28.599 --> 00:31:33.480
<v Speaker 1>of the Newtonian theory. The manuscript of the Principia was

469
00:31:33.519 --> 00:31:38.200
<v Speaker 1>finished by sixteen eighty six. Newton devoted the remainder of

470
00:31:38.240 --> 00:31:41.319
<v Speaker 1>that year to his paper on Physical Optics, the greater

471
00:31:41.480 --> 00:31:44.599
<v Speaker 1>part of which is given up to the subject of diffraction.

472
00:31:45.880 --> 00:31:49.400
<v Speaker 1>In sixteen eighty seven, James the Second having tried to

473
00:31:49.440 --> 00:31:52.720
<v Speaker 1>force the university to admit as a Master of Arts,

474
00:31:53.200 --> 00:31:56.799
<v Speaker 1>a Roman Catholic priest who refused to take oaths of

475
00:31:56.920 --> 00:32:01.039
<v Speaker 1>supremacy and allegiance. Newton took a prominent part in resisting

476
00:32:01.039 --> 00:32:04.119
<v Speaker 1>the illegal interference of the King, and was one of

477
00:32:04.160 --> 00:32:07.480
<v Speaker 1>the deputation sent to London to protect the rights of

478
00:32:07.519 --> 00:32:11.319
<v Speaker 1>the university. The act of partaken by Newton in this

479
00:32:11.400 --> 00:32:15.680
<v Speaker 1>affair led to his being in sixteen eighty nine elected

480
00:32:15.720 --> 00:32:20.640
<v Speaker 1>member for the University. This parliament only lasted thirteen months,

481
00:32:20.680 --> 00:32:25.359
<v Speaker 1>and on its disillusion he gave up his seat. He

482
00:32:25.480 --> 00:32:28.400
<v Speaker 1>was subsequently returned in seventeen oh one, but he never

483
00:32:28.480 --> 00:32:32.880
<v Speaker 1>took any prominent part in politics. On his coming back

484
00:32:32.920 --> 00:32:37.000
<v Speaker 1>to Cambridge in sixteen ninety he resumed his mathematical studies

485
00:32:37.000 --> 00:32:41.759
<v Speaker 1>and correspondence. If he lectured at this time, which is doubtful,

486
00:32:42.279 --> 00:32:45.279
<v Speaker 1>it was on the subject matter of the Principia. The

487
00:32:45.319 --> 00:32:49.559
<v Speaker 1>two letters to Wallace which he explained his methods of

488
00:32:49.599 --> 00:32:53.599
<v Speaker 1>Fluxion's influence, which were written in sixteen ninety two and

489
00:32:53.680 --> 00:32:57.680
<v Speaker 1>published in sixteen ninety three. Towards the close of sixteen

490
00:32:57.759 --> 00:33:01.200
<v Speaker 1>ninety two and throughout the two following year years Newton

491
00:33:01.240 --> 00:33:05.960
<v Speaker 1>had a long illness, suffering from insomnia and general nervous irritability.

492
00:33:06.720 --> 00:33:10.720
<v Speaker 1>Perhaps he never quite regained his elasticity of mind, and

493
00:33:11.000 --> 00:33:14.240
<v Speaker 1>though after his recovery he chewed the same power in

494
00:33:14.319 --> 00:33:19.400
<v Speaker 1>solving any question propounded to him, he ceased there thenceforward

495
00:33:19.880 --> 00:33:23.200
<v Speaker 1>to do original work of his own initiative, and it

496
00:33:23.279 --> 00:33:27.319
<v Speaker 1>was somewhat difficult to stir him to activity in new subjects.

497
00:33:27.839 --> 00:33:31.640
<v Speaker 1>In sixteen ninety four, Newton began to collect data connected

498
00:33:31.680 --> 00:33:34.880
<v Speaker 1>with the irregularities of the moon's motion, with the view

499
00:33:34.960 --> 00:33:38.039
<v Speaker 1>of revising the part of the Principia which dealt with

500
00:33:38.079 --> 00:33:43.680
<v Speaker 1>that subject to render the observations more accurate. He forwarded

501
00:33:43.720 --> 00:33:47.799
<v Speaker 1>to Flamstead a table of corrections for refraction which he

502
00:33:47.839 --> 00:33:52.200
<v Speaker 1>had previously made. This was not published till seventeen twenty one,

503
00:33:52.640 --> 00:33:56.839
<v Speaker 1>when Halley communicated it to the Royal Society. The original

504
00:33:56.880 --> 00:34:00.319
<v Speaker 1>calculations of Newton and the papers connected with it, or

505
00:34:00.319 --> 00:34:03.880
<v Speaker 1>in the Portsmouth Collection, enschw that Newton attained it by

506
00:34:03.880 --> 00:34:07.000
<v Speaker 1>finding the path of array by means of quadratures, in

507
00:34:07.039 --> 00:34:10.039
<v Speaker 1>a manner equivalent to the solution of a differential equation.

508
00:34:10.960 --> 00:34:14.679
<v Speaker 1>As an illustration of Newton's genius. I may mention that

509
00:34:14.719 --> 00:34:18.199
<v Speaker 1>even as late as seventeen fifty four Euler failed to

510
00:34:18.280 --> 00:34:23.480
<v Speaker 1>solve the same problem. In seventeen eighty two, Laplace gave

511
00:34:23.480 --> 00:34:26.679
<v Speaker 1>a rule for constructing such a table, and his results

512
00:34:26.719 --> 00:34:30.519
<v Speaker 1>agree substantially with those of Newton. I do not suppose

513
00:34:30.559 --> 00:34:33.639
<v Speaker 1>that Newton would in any case have produced much more

514
00:34:33.679 --> 00:34:37.760
<v Speaker 1>original work after his illness. But his appointment in sixteen

515
00:34:37.840 --> 00:34:41.719
<v Speaker 1>ninety six as warden and his promotion in sixteen ninety

516
00:34:41.800 --> 00:34:45.000
<v Speaker 1>nine to the mastership of the Mint at a salary

517
00:34:45.000 --> 00:34:48.159
<v Speaker 1>of one thousand, five hundred pounds a year, brought his

518
00:34:48.280 --> 00:34:52.280
<v Speaker 1>scientific investigations to an end, though it was only after

519
00:34:52.400 --> 00:34:55.960
<v Speaker 1>this that many of his previous investigations were published in

520
00:34:55.960 --> 00:34:59.440
<v Speaker 1>the form of books. In sixteen ninety six he moved

521
00:34:59.440 --> 00:35:03.280
<v Speaker 1>to London. In seventeen o one he resigned the Lacasian chair,

522
00:35:03.960 --> 00:35:07.199
<v Speaker 1>and in seventeen o three he was elected President of

523
00:35:07.199 --> 00:35:14.960
<v Speaker 1>the Royal Society. End of section twenty five. Recording by

524
00:35:15.000 --> 00:35:19.880
<v Speaker 1>Paul King, Oakville, Ontario, p J K dot scripts dot

525
00:35:20.000 --> 00:35:22.480
<v Speaker 1>M I T dot E d U forward slash p

526
00:35:22.639 --> 00:35:23.000
<v Speaker 1>K J
