4 THE MEASURE OF THINGS
《万物简史英文版》章节: 4 THE MEASURE OF THINGS,宠文网网友提供全文无弹窗免费在线阅读。!
At the time people had lately become infected with a powerful desire to understand theEarth—to determine how old it was, and how massive, where it hung in space, and how it hadcome to be. The French party’s goal was to help settle the question of the circumference ofthe planet by measuring the length of one degree of meridian (or 1/360 of the distance aroundthe planet) along a line reaching from Yarouqui, near Quito, to just beyond Cuenca in what isnow Ecuador, a distance of about two hundred miles.
1Almost at once things began to go wrong, sometimes spectacularly so. In Quito, the visitorssomehow provoked the locals and were chased out of town by a mob armed with stones. Soonafter, the expedition’s doctor was murdered in a misunderstanding over a woman. Thebotanist became deranged. Others died of fevers and falls. The third most senior member ofthe party, a man named Pierre Godin, ran off with a thirteen-year-old girl and could not beinduced to return.
At one point the group had to suspend work for eight months while La Condamine rode off toLima to sort out a problem with their permits. Eventually he and Bouguer stopped speakingand refused to work together. Everywhere the dwindling party went it was met with thedeepest suspicions from officials who found it difficult to believe that a group of Frenchscientists would travel halfway around the world to measure the world. That made no sense atall. Two and a half centuries later it still seems a reasonable question. Why didn’t the Frenchmake their measurements in France and save themselves all the bother and discomfort of theirAndean adventure?
The answer lies partly with the fact that eighteenth-century scientists, the French in particular,seldom did things simply if an absurdly demanding alternative was available, and partly witha practical problem that had first arisen with the English astronomer Edmond Halley manyyears before—long before Bouguer and La Condamine dreamed of going to South America,much less had a reason for doing so.
* Triangulation, their chosen method, was a popular technique based on the geometric fact that if you know thelength of one side of a triangle and the angles of two corners, you can work out all its other dimensions withoutleaving your chair. Suppose, by way of example, that you and I decided we wished to know how far it is to theMoon. Using triangulation, the first thing we must do is put some distance between us, so lets say for argumentthat you stay in Paris and I go to Moscow and we both look at the Moon at the same time. Now if you imagine aline connecting the three principals of this exercise-that is, you and I and the Moon-it forms a triangle. Measurethe length of the baseline between you and me and the angles of our two corners and the rest can be simplycalculated. (Because the interior angles of a triangle always add up to 180 degrees, if you know the sum of twoof the angles you can instantly calculate the third; and knowing the precise shape of a triangle and the length ofone side tells you the lengths of the other sides.) This was in fact the method use by a Greek astronomer,Hipparchus of Nicaea, in 150 B.C. to work out the Moons distance from Earth. At ground level, the principles oftriangulation are the same, except that the triangles dont reach into space but rather are laid side to side on amap. In measuring a degree of meridian, the surveyors would create a sort of chain of triangles marching acrossthe landscape.
Halley was an exceptional figure. In the course of a long and productive career, he was asea captain, a cartographer, a professor of geometry at the University of Oxford, deputycontroller of the Royal Mint, astronomer royal, and inventor of the deep-sea diving bell. Hewrote authoritatively on magnetism, tides, and the motions of the planets, and fondly on theeffects of opium. He invented the weather map and actuarial table, proposed methods forworking out the age of the Earth and its distance from the Sun, even devised a practicalmethod for keeping fish fresh out of season. The one thing he didn’t do, interestingly enough,was discover the comet that bears his name. He merely recognized that the comet he saw in1682 was the same one that had been seen by others in 1456, 1531, and 1607. It didn’tbecome Halley’s comet until 1758, some sixteen years after his death.
For all his achievements, however, Halley’s greatest contribution to human knowledge maysimply have been to take part in a modest scientific wager with two other worthies of his day:
Robert Hooke, who is perhaps best remembered now as the first person to describe a cell, andthe great and stately Sir Christopher Wren, who was actually an astronomer first and architectsecond, though that is not often generally remembered now. In 1683, Halley, Hooke, andWren were dining in London when the conversation turned to the motions of celestial objects.
It was known that planets were inclined to orbit in a particular kind of oval known as anellipse—“a very specific and precise curve,” to quote Richard Feynman—but it wasn’tunderstood why. Wren generously offered a prize worth forty shillings (equivalent to a coupleof weeks’ pay) to whichever of the men could provide a solution.
Hooke, who was well known for taking credit for ideas that weren’t necessarily his own,claimed that he had solved the problem already but declined now to share it on the interestingand inventive grounds that it would rob others of the satisfaction of discovering the answer forthemselves. He would instead “conceal it for some time, that others might know how to valueit.” If he thought any more on the matter, he left no evidence of it. Halley, however, becameconsumed with finding the answer, to the point that the following year he traveled toCambridge and boldly called upon the university’s Lucasian Professor of Mathematics, IsaacNewton, in the hope that he could help.
Newton was a decidedly odd figure—brilliant beyond measure, but solitary, joyless, pricklyto the point of paranoia, famously distracted (upon swinging his feet out of bed in the morninghe would reportedly sometimes sit for hours, immobilized by the sudden rush of thoughts tohis head), and capable of the most riveting strangeness. He built his own laboratory, the firstat Cambridge, but then engaged in the most bizarre experiments. Once he inserted a bodkin—a long needle of the sort used for sewing leather—into his eye socket and rubbed it around“betwixt my eye and the bone as near to [the] backside of my eye as I could” just to see whatwould happen. What happened, miraculously, was nothing—at least nothing lasting. Onanother occasion, he stared at the Sun for as long as he could bear, to determine what effect itwould have upon his vision. Again he escaped lasting damage, though he had to spend somedays in a darkened room before his eyes forgave him.
Set atop these odd beliefs and quirky traits, however, was the mind of a supreme genius—though even when working in conventional channels he often showed a tendency topeculiarity. As a student, frustrated by the limitations of conventional mathematics, heinvented an entirely new form, the calculus, but then told no one about it for twenty-sevenyears. In like manner, he did work in optics that transformed our understanding of light andlaid the foundation for the science of spectroscopy, and again chose not to share the results forthree decades.
For all his brilliance, real science accounted for only a part of his interests. At least half hisworking life was given over to alchemy and wayward religious pursuits. These were not meredabblings but wholehearted devotions. He was a secret adherent of a dangerously hereticalsect called Arianism, whose principal tenet was the belief that there had been no Holy Trinity(slightly ironic since Newton’s college at Cambridge was Trinity). He spent endless hoursstudying the floor plan of the lost Temple of King Solomon in Jerusalem (teaching himselfHebrew in the process, the better to scan original texts) in the belief that it held mathematicalclues to the dates of the second coming of Christ and the end of the world. His attachment toalchemy was no less ardent. In 1936, the economist John Maynard Keynes bought a trunk ofNewton’s papers at auction and discovered with astonishment that they were overwhelminglypreoccupied not with optics or planetary motions, but with a single-minded quest to turn basemetals into precious ones. An analysis of a strand of Newton’s hair in the 1970s found itcontained mercury—an element of interest to alchemists, hatters, and thermometer-makersbut almost no one else—at a concentration some forty times the natural level. It is perhapslittle wonder that he had trouble remembering to rise in the morning.
Quite what Halley expected to get from him when he made his unannounced visit in August1684 we can only guess. But thanks to the later account of a Newton confidant, AbrahamDeMoivre, we do have a record of one of science’s most historic encounters:
In 1684 DrHalley came to visit at Cambridge [and] after they had some timetogether the Drasked him what he thought the curve would be that would bedescribed by the Planets supposing the force of attraction toward the Sun to bereciprocal to the square of their distance from it.
This was a reference to a piece of mathematics known as the inverse square law, which Halleywas convinced lay at the heart of the explanation, though he wasn’t sure exactly how.
SrIsaac replied immediately that it would be an [ellipse]. The Doctor, struck withjoy & amazement, asked him how he knew it. ‘Why,’ saith he, ‘I have calculatedit,’ whereupon DrHalley asked him for his calculation without farther delay,SrIsaac looked among his papers but could not find it.
This was astounding—like someone saying he had found a cure for cancer but couldn’tremember where he had put the formula. Pressed by Halley, Newton agreed to redo thecalculations and produce a paper. He did as promised, but then did much more. He retired fortwo years of intensive reflection and scribbling, and at length produced his masterwork: thePhilosophiae Naturalis Principia Mathematica or Mathematical Principles of NaturalPhilosophy, better known as the Principia .
Once in a great while, a few times in history, a human mind produces an observation soacute and unexpected that people can’t quite decide which is the more amazing—the fact orthe thinking of it. Principia was one of those moments. It made Newton instantly famous. For the rest of his life he would be draped with plaudits and honors, becoming, among much else,the first person in Britain knighted for scientific achievement. Even the great Germanmathematician Gottfried von Leibniz, with whom Newton had a long, bitter fight over priorityfor the invention of the calculus, thought his contributions to mathematics equal to all theaccumulated work that had preceded him. “Nearer the gods no mortal may approach,” wroteHalley in a sentiment that was endlessly echoed by his contemporaries and by many otherssince.
Although the Principia has been called “one of the most inaccessible books ever written”
(Newton intentionally made it difficult so that he wouldn’t be pestered by mathematical“smatterers,” as he called them), it was a beacon to those who could follow it. It not onlyexplained mathematically the orbits of heavenly bodies, but also identified the attractive forcethat got them moving in the first place—gravity. Suddenly every motion in the universe madesense.
At Principia ’s heart were Newton’s three laws of motion (which state, very baldly, that athing moves in the direction in which it is pushed; that it will keep moving in a straight lineuntil some other force acts to slow or deflect it; and that every action has an opposite andequal reaction) and his universal law of gravitation. This states that every object in theuniverse exerts a tug on every other. It may not seem like it, but as you sit here now you arepulling everything around you—walls, ceiling, lamp, pet cat—toward you with your own little(indeed, very little) gravitational field. And these things are also pulling on you. It wasNewton who realized that the pull of any two objects is, to quote Feynman again,“proportional to the mass of each and varies inversely as the square of the distance betweenthem.” Put another way, if you double the distance between two objects, the attractionbetween them becomes four times weaker. This can be expressed with the formulaF = GmmR2which is of course way beyond anything that most of us could make practical use of, but atleast we can appreciate that it is elegantly compact. A couple of brief multiplications, a simpledivision, and, bingo, you know your gravitational position wherever you go. It was the firstreally universal law of nature ever propounded by a human mind, which is why Newton isregarded with such universal esteem.
Principia’s production was not without drama. To Halley’s horror, just as work wasnearing completion Newton and Hooke fell into dispute over the priority for the inversesquare law and Newton refused to release the crucial third volume, without which the firsttwo made little sense. Only with some frantic shuttle diplomacy and the most liberalapplications of flattery did Halley manage finally to extract the concluding volume from theerratic professor.
Halley’s traumas were not yet quite over. The Royal Society had promised to publish thework, but now pulled out, citing financial embarrassment. The year before the society hadbacked a costly flop called The History of Fishes , and they now suspected that the market fora book on mathematical principles would be less than clamorous. Halley, whose means werenot great, paid for the book’s publication out of his own pocket. Newton, as was his custom,contributed nothing. To make matters worse, Halley at this time had just accepted a positionas the society’s clerk, and he was informed that the society could no longer afford to provide him with a promised salary of ￡50 per annum. He was to be paid instead in copies of TheHistory of Fishes .
Newton’s laws explained so many things—the slosh and roll of ocean tides, the motions ofplanets, why cannonballs trace a particular trajectory before thudding back to Earth, why wearen’t flung into space as the planet spins beneath us at hundreds of miles an hour2—that ittook a while for all their implications to seep in. But one revelation became almostimmediately controversial.
This was the suggestion that the Earth is not quite round. According to Newton’s theory,the centrifugal force of the Earth’s spin should result in a slight flattening at the poles and abulging at the equator, which would make the planet slightly oblate. That meant that thelength of a degree wouldn’t be the same in Italy as it was in Scotland. Specifically, the lengthwould shorten as you moved away from the poles. This was not good news for those peoplewhose measurements of the Earth were based on the assumption that the Earth was a perfectsphere, which was everyone.
For half a century people had been trying to work out the size of the Earth, mostly bymaking very exacting measurements. One of the first such attempts was by an Englishmathematician named Richard Norwood. As a young man Norwood had traveled to Bermudawith a diving bell modeled on Halley’s device, intending to make a fortune scooping pearlsfrom the seabed. The scheme failed because there were no pearls and anyway Norwood’s belldidn’t work, but Norwood was not one to waste an experience. In the early seventeenthcentury Bermuda was well known among ships’ captains for being hard to locate. Theproblem was that the ocean was big, Bermuda small, and the navigational tools for dealingwith this disparity hopelessly inadequate. There wasn’t even yet an agreed length for anautical mile. Over the breadth of an ocean the smallest miscalculations would becomemagnified so that ships often missed Bermuda-sized targets by dismaying margins. Norwood,whose first love was trigonometry and thus angles, decided to bring a little mathematical rigorto navigation and to that end he determined to calculate the length of a degree.
Starting with his back against the Tower of London, Norwood spent two devoted yearsmarching 208 miles north to York, repeatedly stretching and measuring a length of chain ashe went, all the while making the most meticulous adjustments for the rise and fall of the landand the meanderings of the road. The final step was to measure the angle of the Sun at York atthe same time of day and on the same day of the year as he had made his first measurement inLondon. From this, he reasoned he could determine the length of one degree of the Earth’smeridian and thus calculate the distance around the whole. It was an almost ludicrouslyambitious undertaking—a mistake of the slightest fraction of a degree would throw the wholething out by miles—but in fact, as Norwood proudly declaimed, he was accurate to “within ascantling”—or, more precisely, to within about six hundred yards. In metric terms, his figureworked out at 110.72 kilometers per degree of arc.
In 1637, Norwood’s masterwork of navigation, The Seaman’s Practice , was published andfound an immediate following. It went through seventeen editions and was still in printtwenty-five years after his death. Norwood returned to Bermuda with his family, becoming a2How fast you are spinning depends on where you are. The speed of the Earth’s spin varies from a little over1,000 miles an hour at the equator to 0 at the poles.
successful planter and devoting his leisure hours to his first love, trigonometry. He survivedthere for thirty-eight years and it would be pleasing to report that he passed this span inhappiness and adulation. In fact, he didn’t. On the crossing from England, his two young sonswere placed in a cabin with the Reverend Nathaniel White, and somehow so successfullytraumatized the young vicar that he devoted much of the rest of his career to persecutingNorwood in any small way he could think of.
Norwood’s two daughters brought their father additional pain by making poor marriages.
One of the husbands, possibly incited by the vicar, continually laid small charges againstNorwood in court, causing him much exasperation and necessitating repeated trips acrossBermuda to defend himself. Finally in the 1650s witch trials came to Bermuda and Norwoodspent his final years in severe unease that his papers on trigonometry, with their arcanesymbols, would be taken as communications with the devil and that he would be treated to adreadful execution. So little is known of Norwood that it may in fact be that he deserved hisunhappy declining years. What is certainly true is that he got them.
Meanwhile, the momentum for determining the Earth’s circumference passed to France.
There, the astronomer Jean Picard devised an impressively complicated method oftriangulation involving quadrants, pendulum clocks, zenith sectors, and telescopes (forobserving the motions of the moons of Jupiter). After two years of trundling and triangulatinghis way across France, in 1669 he announced a more accurate measure of 110.46 kilometersfor one degree of arc. This was a great source of pride for the French, but it was predicated onthe assumption that the Earth was a perfect sphere—which Newton now said it was not.
To complicate matters, after Picard’s death the father-and-son team of Giovanni andJacques Cassini repeated Picard’s experiments over a larger area and came up with results thatsuggested that the Earth was fatter not at the equator but at the poles—that Newton, in otherwords, was exactly wrong. It was this that prompted the Academy of Sciences to dispatchBouguer and La Condamine to South America to take new measurements.
They chose the Andes because they needed to measure near the equator, to determine ifthere really was a difference in sphericity there, and because they reasoned that mountainswould give them good sightlines. In fact, the mountains of Peru were so constantly lost incloud that the team often had to wait weeks for an hour’s clear surveying. On top of that, theyhad selected one of the most nearly impossible terrains on Earth. Peruvians refer to theirlandscape as muy accidentado —“much accidented”—and this it most certainly is. TheFrench had not only to scale some of the world’s most challenging mountains—mountainsthat defeated even their mules—but to reach the mountains they had to ford wild rivers, hacktheir way through jungles, and cross miles of high, stony desert, nearly all of it uncharted andfar from any source of supplies. But Bouguer and La Condamine were nothing if nottenacious, and they stuck to the task for nine and a half long, grim, sun-blistered years.
Shortly before concluding the project, they received word that a second French team, takingmeasurements in northern Scandinavia (and facing notable discomforts of their own, fromsquelching bogs to dangerous ice floes), had found that a degree was in fact longer near thepoles, as Newton had promised. The Earth was forty-three kilometers stouter when measuredequatorially than when measured from top to bottom around the poles.
Bouguer and La Condamine thus had spent nearly a decade working toward a result theydidn’t wish to find only to learn now that they weren’t even the first to find it. Listlessly, they completed their survey, which confirmed that the first French team was correct. Then, still notspeaking, they returned to the coast and took separate ships home.
Something else conjectured by Newton in the Principia was that a plumb bob hung near amountain would incline very slightly toward the mountain, affected by the mountain’sgravitational mass as well as by the Earth’s. This was more than a curious fact. If youmeasured the deflection accurately and worked out the mass of the mountain, you couldcalculate the universal gravitational constant—that is, the basic value of gravity, known asG—and along with it the mass of the Earth.
Bouguer and La Condamine had tried this on Peru’s Mount Chimborazo, but had beendefeated by both the technical difficulties and their own squabbling, and so the notion laydormant for another thirty years until resurrected in England by Nevil Maskelyne, theastronomer royal. In Dava Sobel’s popular book Longitude, Maskelyne is presented as a ninnyand villain for failing to appreciate the brilliance of the clockmaker John Harrison, and thismay be so, but we are indebted to him in other ways not mentioned in her book, not least forhis successful scheme to weigh the Earth. Maskelyne realized that the nub of the problem laywith finding a mountain of sufficiently regular shape to judge its mass.
At his urging, the Royal Society agreed to engage a reliable figure to tour the British Islesto see if such a mountain could be found. Maskelyne knew just such a person—theastronomer and surveyor Charles Mason. Maskelyne and Mason had become friends elevenyears earlier while engaged in a project to measure an astronomical event of great importance:
the passage of the planet Venus across the face of the Sun. The tireless Edmond Halley hadsuggested years before that if you measured one of these passages from selected points on theEarth, you could use the principles of triangulation to work out the distance to the Sun, andfrom that calibrate the distances to all the other bodies in the solar system.
Unfortunately, transits of Venus, as they are known, are an irregular occurrence. Theycome in pairs eight years apart, but then are absent for a century or more, and there were nonein Halley’s lifetime.
3But the idea simmered and when the next transit came due in 1761,nearly two decades after Halley’s death, the scientific world was ready—indeed, more readythan it had been for an astronomical event before.
With the instinct for ordeal that characterized the age, scientists set off for more than ahundred locations around the globe—to Siberia, China, South Africa, Indonesia, and thewoods of Wisconsin, among many others. France dispatched thirty-two observers, Britaineighteen more, and still others set out from Sweden, Russia, Italy, Germany, Ireland, andelsewhere.
It was history’s first cooperative international scientific venture, and almost everywhere itran into problems. Many observers were waylaid by war, sickness, or shipwreck. Others madetheir destinations but opened their crates to find equipment broken or warped by tropical heat.
Once again the French seemed fated to provide the most memorably unlucky participants.
Jean Chappe spent months traveling to Siberia by coach, boat, and sleigh, nursing his delicateinstruments over every perilous bump, only to find the last vital stretch blocked by swollen3The next transit will be on June 8, 2004, with a second in 2012. There were none in the twentieth century.
rivers, the result of unusually heavy spring rains, which the locals were swift to blame on himafter they saw him pointing strange instruments at the sky. Chappe managed to escape withhis life, but with no useful measurements.
Unluckier still was Guillaume Le Gentil, whose experiences are wonderfully summarizedby Timothy Ferris in Coming of Age in the Milky Way . Le Gentil set off from France a yearahead of time to observe the transit from India, but various setbacks left him still at sea on theday of the transit—just about the worst place to be since steady measurements wereimpossible on a pitching ship.
Undaunted, Le Gentil continued on to India to await the next transit in 1769. With eightyears to prepare, he erected a first-rate viewing station, tested and retested his instruments,and had everything in a state of perfect readiness. On the morning of the second transit, June4, 1769, he awoke to a fine day, but, just as Venus began its pass, a cloud slid in front of theSun and remained there for almost exactly the duration of the transit: three hours, fourteenminutes, and seven seconds.
Stoically, Le Gentil packed up his instruments and set off for the nearest port, but en routehe contracted dysentery and was laid up for nearly a year. Still weakened, he finally made itonto a ship. It was nearly wrecked in a hurricane off the African coast. When at last hereached home, eleven and a half years after setting off, and having achieved nothing, hediscovered that his relatives had had him declared dead in his absence and hadenthusiastically plundered his estate.
In comparison, the disappointments experienced by Britain’s eighteen scattered observerswere mild. Mason found himself paired with a young surveyor named Jeremiah Dixon andapparently they got along well, for they formed a lasting partnership. Their instructions wereto travel to Sumatra and chart the transit there, but after just one night at sea their ship wasattacked by a French frigate. (Although scientists were in an internationally cooperativemood, nations weren’t.) Mason and Dixon sent a note to the Royal Society observing that itseemed awfully dangerous on the high seas and wondering if perhaps the whole thingoughtn’t to be called off. In reply they received a swift and chilly rebuke, noting that they hadalready been paid, that the nation and scientific community were counting on them, and thattheir failure to proceed would result in the irretrievable loss of their reputations. Chastened,they sailed on, but en route word reached them that Sumatra had fallen to the French and sothey observed the transit inconclusively from the Cape of Good Hope. On the way home theystopped on the lonely Atlantic outcrop of St. Helena, where they met Maskelyne, whoseobservations had been thwarted by cloud cover. Mason and Maskelyne formed a solidfriendship and spent several happy, and possibly even mildly useful, weeks charting tidalflows.
Soon afterward, Maskelyne returned to England where he became astronomer royal, andMason and Dixon—now evidently more seasoned—set off for four long and often perilousyears surveying their way through 244 miles of dangerous American wilderness to settle aboundary dispute between the estates of William Penn and Lord Baltimore and theirrespective colonies of Pennsylvania and Maryland. The result was the famous Mason andDixon line, which later took on symbolic importance as the dividing line between the slaveand free states. (Although the line was their principal task, they also contributed severalastronomical surveys, including one of the century’s most accurate measurements of a degree of meridian—an achievement that brought them far more acclaim in England than the settlingof a boundary dispute between spoiled aristocrats.)Back in Europe, Maskelyne and his counterparts in Germany and France were forced to theconclusion that the transit measurements of 1761 were essentially a failure. One of theproblems, ironically, was that there were too many observations, which when broughttogether often proved contradictory and impossible to resolve. The successful charting of aVenusian transit fell instead to a little-known Yorkshire-born sea captain named James Cook,who watched the 1769 transit from a sunny hilltop in Tahiti, and then went on to chart andclaim Australia for the British crown. Upon his return there was now enough information forthe French astronomer Joseph Lalande to calculate that the mean distance from the Earth tothe Sun was a little over 150 million kilometers. (Two further transits in the nineteenthcentury allowed astronomers to put the figure at 149.59 million kilometers, where it hasremained ever since. The precise distance, we now know, is 149.597870691 millionkilometers.) The Earth at last had a position in space.
As for Mason and Dixon, they returned to England as scientific heroes and, for reasonsunknown, dissolved their partnership. Considering the frequency with which they turn up atseminal events in eighteenth-century science, remarkably little is known about either man. Nolikenesses exist and few written references. Of Dixon the Dictionary of National Biographynotes intriguingly that he was “said to have been born in a coal mine,” but then leaves it to thereader’s imagination to supply a plausible explanatory circumstance, and adds that he died atDurham in 1777. Apart from his name and long association with Mason, nothing more isknown.
Mason is only slightly less shadowy. We know that in 1772, at Maskelyne’s behest, heaccepted the commission to find a suitable mountain for the gravitational deflectionexperiment, at length reporting back that the mountain they needed was in the central ScottishHighlands, just above Loch Tay, and was called Schiehallion. Nothing, however, wouldinduce him to spend a summer surveying it. He never returned to the field again. His nextknown movement was in 1786 when, abruptly and mysteriously, he turned up in Philadelphiawith his wife and eight children, apparently on the verge of destitution. He had not been backto America since completing his survey there eighteen years earlier and had no known reasonfor being there, or any friends or patrons to greet him. A few weeks later he was dead.
With Mason refusing to survey the mountain, the job fell to Maskelyne. So for four monthsin the summer of 1774, Maskelyne lived in a tent in a remote Scottish glen and spent his daysdirecting a team of surveyors, who took hundreds of measurements from every possibleposition. To find the mass of the mountain from all these numbers required a great deal oftedious calculating, for which a mathematician named Charles Hutton was engaged. Thesurveyors had covered a map with scores of figures, each marking an elevation at some pointon or around the mountain. It was essentially just a confusing mass of numbers, but Huttonnoticed that if he used a pencil to connect points of equal height, it all became much moreorderly. Indeed, one could instantly get a sense of the overall shape and slope of the mountain.
He had invented contour lines.
Extrapolating from his Schiehallion measurements, Hutton calculated the mass of the Earthat 5,000 million million tons, from which could reasonably be deduced the masses of all theother major bodies in the solar system, including the Sun. So from this one experiment welearned the masses of the Earth, the Sun, the Moon, the other planets and their moons, and gotcontour lines into the bargain—not bad for a summer’s work.
Not everyone was satisfied with the results, however. The shortcoming of the Schiehallionexperiment was that it was not possible to get a truly accurate figure without knowing theactual density of the mountain. For convenience, Hutton had assumed that the mountain hadthe same density as ordinary stone, about 2.5 times that of water, but this was little more thanan educated guess.
One improbable-seeming person who turned his mind to the matter was a country parsonnamed John Michell, who resided in the lonely Yorkshire village of Thornhill. Despite hisremote and comparatively humble situation, Michell was one of the great scientific thinkers ofthe eighteenth century and much esteemed for it.
Among a great deal else, he perceived the wavelike nature of earthquakes, conducted muchoriginal research into magnetism and gravity, and, quite extraordinarily, envisioned thepossibility of black holes two hundred years before anyone else—a leap of intuitive deductionthat not even Newton could make. When the German-born musician William Herscheldecided his real interest in life was astronomy, it was Michell to whom he turned forinstruction in making telescopes, a kindness for which planetary science has been in his debtever since.
4But of all that Michell accomplished, nothing was more ingenious or had greater impactthan a machine he designed and built for measuring the mass of the Earth. Unfortunately, hedied before he could conduct the experiments and both the idea and the necessary equipmentwere passed on to a brilliant but magnificently retiring London scientist named HenryCavendish.
Cavendish is a book in himself. Born into a life of sumptuous privilege—his grandfatherswere dukes, respectively, of Devonshire and Kent—he was the most gifted English scientistof his age, but also the strangest. He suffered, in the words of one of his few biographers,from shyness to a “degree bordering on disease.” Any human contact was for him a source ofthe deepest discomfort.
Once he opened his door to find an Austrian admirer, freshly arrived from Vienna, on thefront step. Excitedly the Austrian began to babble out praise. For a few moments Cavendishreceived the compliments as if they were blows from a blunt object and then, unable to takeany more, fled down the path and out the gate, leaving the front door wide open. It was somehours before he could be coaxed back to the property. Even his housekeeper communicatedwith him by letter.
Although he did sometimes venture into society—he was particularly devoted to the weeklyscientific soirées of the great naturalist Sir Joseph Banks—it was always made clear to theother guests that Cavendish was on no account to be approached or even looked at. Thosewho sought his views were advised to wander into his vicinity as if by accident and to “talk as4In 1781 Herschel became the first person in the modern era to discover a planet. He wanted to call it George,after the British monarch, but was overruled. Instead it became Uranus.
it were into vacancy.” If their remarks were scientifically worthy they might receive amumbled reply, but more often than not they would hear a peeved squeak (his voice appearsto have been high pitched) and turn to find an actual vacancy and the sight of Cavendishfleeing for a more peaceful corner.
His wealth and solitary inclinations allowed him to turn his house in Clapham into a largelaboratory where he could range undisturbed through every corner of the physical sciences—electricity, heat, gravity, gases, anything to do with the composition of matter. The secondhalf of the eighteenth century was a time when people of a scientific bent grew intenselyinterested in the physical properties of fundamental things—gases and electricity inparticular—and began seeing what they could do with them, often with more enthusiasm thansense. In America, Benjamin Franklin famously risked his life by flying a kite in an electricalstorm. In France, a chemist named Pilatre de Rozier tested the flammability of hydrogen bygulping a mouthful and blowing across an open flame, proving at a stroke that hydrogen isindeed explosively combustible and that eyebrows are not necessarily a permanent feature ofone’s face. Cavendish, for his part, conducted experiments in which he subjected himself tograduated jolts of electrical current, diligently noting the increasing levels of agony until hecould keep hold of his quill, and sometimes his consciousness, no longer.
In the course of a long life Cavendish made a string of signal discoveries—among muchelse he was the first person to isolate hydrogen and the first to combine hydrogen and oxygento form water—but almost nothing he did was entirely divorced from strangeness. To thecontinuing exasperation of his fellow scientists, he often alluded in published work to theresults of contingent experiments that he had not told anyone about. In his secretiveness hedidn’t merely resemble Newton, but actively exceeded him. His experiments with electricalconductivity were a century ahead of their time, but unfortunately remained undiscovereduntil that century had passed. Indeed the greater part of what he did wasn’t known until thelate nineteenth century when the Cambridge physicist James Clerk Maxwell took on the taskof editing Cavendish’s papers, by which time credit had nearly always been given to others.
Among much else, and without telling anyone, Cavendish discovered or anticipated the lawof the conservation of energy, Ohm’s law, Dalton’s Law of Partial Pressures, Richter’s Lawof Reciprocal Proportions, Charles’s Law of Gases, and the principles of electricalconductivity. That’s just some of it. According to the science historian J. G. Crowther, he alsoforeshadowed “the work of Kelvin and G. H. Darwin on the effect of tidal friction on slowingthe rotation of the earth, and Larmor’s discovery, published in 1915, on the effect of localatmospheric cooling . . . the work of Pickering on freezing mixtures, and some of the work ofRooseboom on heterogeneous equilibria.” Finally, he left clues that led directly to thediscovery of the group of elements known as the noble gases, some of which are so elusivethat the last of them wasn’t found until 1962. But our interest here is in Cavendish’s lastknown experiment when in the late summer of 1797, at the age of sixty-seven, he turned hisattention to the crates of equipment that had been left to him—evidently out of simplescientific respect—by John Michell.
When assembled, Michell’s apparatus looked like nothing so much as an eighteenth-century version of a Nautilus weight-training machine. It incorporated weights,counterweights, pendulums, shafts, and torsion wires. At the heart of the machine were two350-pound lead balls, which were suspended beside two smaller spheres. The idea was tomeasure the gravitational deflection of the smaller spheres by the larger ones, which would allow the first measurement of the elusive force known as the gravitational constant, and fromwhich the weight (strictly speaking, the mass)5of the Earth could be deduced.
Because gravity holds planets in orbit and makes falling objects land with a bang, we tendto think of it as a powerful force, but it is not really. It is only powerful in a kind of collectivesense, when one massive object, like the Sun, holds on to another massive object, like theEarth. At an elemental level gravity is extraordinarily unrobust. Each time you pick up a bookfrom a table or a dime from the floor you effortlessly overcome the combined gravitationalexertion of an entire planet. What Cavendish was trying to do was measure gravity at thisextremely featherweight level.
Delicacy was the key word. Not a whisper of disturbance could be allowed into the roomcontaining the apparatus, so Cavendish took up a position in an adjoining room and made hisobservations with a telescope aimed through a peephole. The work was incredibly exactingand involved seventeen delicate, interconnected measurements, which together took nearly ayear to complete. When at last he had finished his calculations, Cavendish announced that theEarth weighed a little over 13,000,000,000,000,000,000,000 pounds, or six billion trillionmetric tons, to use the modern measure. (A metric ton is 1,000 kilograms or 2,205 pounds.)Today, scientists have at their disposal machines so precise they can detect the weight of asingle bacterium and so sensitive that readings can be disturbed by someone yawning seventy-five feet away, but they have not significantly improved on Cavendish’s measurements of1797. The current best estimate for Earth’s weight is 5.9725 billion trillion metric tons, adifference of only about 1 percent from Cavendish’s finding. Interestingly, all of this merelyconfirmed estimates made by Newton 110 years before Cavendish without any experimentalevidence at all.
So, by the late eighteenth century scientists knew very precisely the shape and dimensionsof the Earth and its distance from the Sun and planets; and now Cavendish, without evenleaving home, had given them its weight. So you might think that determining the age of theEarth would be relatively straightforward. After all, the necessary materials were literally attheir feet. But no. Human beings would split the atom and invent television, nylon, and instantcoffee before they could figure out the age of their own planet.
To understand why, we must travel north to Scotland and begin with a brilliant and genialman, of whom few have ever heard, who had just invented a new science called geology.
5To a physicist, mass and weight are two quite different things. Your mass stays the same wherever you go, butyour weight varies depending on how far you are from the center of some other massive object like a planet.
Travel to the Moon and you will be much lighter but no less massive.