Examining the History, Navigation, and Landfall of Christopher Columbus
This and related pages copyright © 1997-2010 by Keith A. Pickering
|Columbus and dead reckoning navigation.|
|Columbus and celestial navigation.|
|How long was Columbus’s league? And how large was his Earth?|
|Columbus and longitude.|
|Where was Columbus’s first landing place in the New World? Visit the Columbus Landfall Homepage.|
|A Columbus Timeline.|
|Columbus’s early years, 1451-1492.|
|The First Voyage, 1492-1493.|
|The Second Voyage, 1493-1496.|
|The Third Voyage, 1498-1500.|
|The Fourth Voyage, 1502-1504.|
|Columbus’s death and burial.|
Columbus Special Topics
|Who really discovered America?|
|Columbus and the destruction of native peoples.|
|The Columbus Landfall Homepage.|
|A select bibliography of Columbus literature, with capsule reviews.|
|Want to know more? Try these Links to other sites about Columbus and his times.|
|Search The Columbus Navigation and Landfall pages.|
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Columbus and Celestial Navigation
Although Columbus was primarily a dead reckoning navigator, he did experiment with celestial navigation techniques from time to time. However, these experiments were usually unsuccessful — and in some cases, actually fraudulent.
In celestial navigation, the navigator observes celestial bodies (Sun, Moon, and stars) to measure his latitude. (In Columbus’s day, it was usually impossible to measure your longitude.) Even in ancient times, it was fairly easy to find your latitude by looking at the Sun and stars, as long as you weren’t too concerned about accuracy. Each star has a celestial latitude or declination. If you know the declination of a star that is directly overhead, that’s the same as your latitude on earth. Even if a star isn’t directly overhead, if you can measure the angle between the star and the overhead point (called the zenith), you can still determine your latitude that way — provided you measure the star at the time of night that it is highest in the sky.
But in the Mediterranean Sea, it’s not very useful to find your latitude, because your latitude is roughly the same wherever you are. In those confined waters, dead reckoning was the easiest way to navigate. It was not until the fifteenth century, when Portuguese mariners began to make long voyages north and south along the coast of Africa, that celestial determination of latitude began to be useful for southern European sailors.
Columbus was from Genoa, one of the leading Mediterranean ports, and he must have learned his dead reckoning navigation from Genoese pilots. But he had spent time in Portugal and was aware of all the new ideas in navigation, including celestial navigation. So on his first voyage, he made at least five separate attempts to measure his latitude using celestial methods. Not one of these attempts was successful, in part because of bad luck, and in part because of Columbus’s own ignorance of celestial techniques and tools.
2. The tools.
The most important tool used by Columbus in his celestial attempts was the quadrant. This was a metal plate in the shape of a quarter-circle. From the center of the circle hung a weight on a string, that crossed the opposite edge of the circle (see figure 1). The navigator would sight the North Star along one edge, and the point that the string crossed the edge would show the star’s altitude or angle above the horizon. (In the case of the North Star, this is always pretty close to your latitude). Many examples of quadrants survive in maritime museums, and often have several scales along the edge. For example, in addition to the angle, you might also read the tangent of the angle from the quadrant. The tangent scale is useful if the quadrant is to be used for architectural purposes.
Columbus also carried an astrolabe on the first voyage, which is somewhat similar to the quadrant. The astrolabe was a complete circle of metal and had a moving arm (or alidade) that the navigator would sight along to find the star’s altitude. Columbus tried to use the astrolabe once but was stymied by bad weather, and he never used it again. Both the quadrant and astrolabe are dependent upon gravity to work, so they can measure only vertical angles. The quadrant was accurate to about a degree or so, and the astrolabe was a little less accurate.
Time aboard ship was measured by a sandglass (or in Spanish, ampoletta). It was the responsibility of the ship’s boy to turn the glass every half-hour in order to measure the time until the watch changed. Since the sandglass was always running a little slow or fast, it was checked daily against the times of sunrise, sunset, or midnight. Midnight could be determined by using a nocturnal, a nifty little tool which tells the time of the night by the rotation of stars around the celestial pole.
3. The First Voyage Failures.
After navigating successfully across the Atlantic using his familiar dead reckoning methods, Columbus tried to find his latitude using the quadrant on October 30, 1492. At the time, he was at Puerto de Mares, Cuba, probably the modern Nuevitas, at about 21° 30′ North latitude. But the result he obtained from the quadrant was 42 degrees. He made another reading from the same place on November 2 and got the same flawed result.
Continuing along the coast of Cuba, Columbus again tried a quadrant latitude reading on November 21, and again came up with 42 degrees. Columbus was by now aware that the quadrant reading was incorrect, but he dutifully recorded the reading in his log anyway — he blamed the quadrant for the bad result and remarked that he would not take any more readings until the quadrant could be fixed.
Columbus made two separate attempts to measure his latitude by two different methods on December 13, while anchored in a harbor in northern Haiti. Columbus had read works by the Greek astronomer Ptolemy, and he knew that Ptolemy often referred to a city’s latitude according to the length of daylight at the summer solstice (more northerly places have longer daylight at summer solstice). December 13 was the day after the winter solstice in 1492, which is just as good for latitude measurements (because the length of daylight at summer solstice is about the same as the length of the night at the winter solstice). Columbus took the opportunity to measure the length of daylight, finding that the day was 10 hours long. This is also a fairly bad result, but Columbus did not convert the daylight measurement into a latitude, probably because he did not know enough trigonometry to do so.
That night, he made his second attempt to determine latitude within 24 hours. Going back to the quadrant, he again tried to determine the altitude of the North Star, and this time got a reading of 34 degrees — still far from his correct latitude of 19 degrees.
Finally, on February 3, 1493, while on the return voyage, Columbus tried to determine the altitude of Polaris using both the quadrant and astrolabe; but the waves were so high he could not get a reading.
The quadrant readings Columbus obtained on his first voyage are horrible by any standard. Some have suggested that Columbus mistook another star for Polaris, but that seems ridiculous: Columbus used the stars of Ursa Minor to tell time at night, so he was very familiar with that constellation. In 1983, James E. Kelley, Jr. provided the solution to the mystery: as mentioned above, many quadrants in maritime museums have tangent scales. If Columbus misread the scale, he might have recorded the tangent of his latitude (without the decimal point) instead of his actual latitude. If that were the case, Columbus’s measurements would only be wrong by a couple of degrees or so, which is not bad considering the technology.
In any case, it is clear that at this point in his career Columbus was not familiar enough with celestial techniques and tools to use them successfully. So it is not surprising that on his second voyage, there is no record that Columbus attempted to use celestial navigation (except for the fraudulent eclipse longitudes). Instead, he stuck to the tried and true dead reckoning practice of “rhumbline sailing”, keeping a constant west-by-south course the whole way from Gomera to Dominica in the West Indies.
4. The Third Voyage: Some Improvements?
In 1498, Columbus sailed from Spain with six ships of supplies for the settlers on Hispaniola. This is the only voyage on which Columbus made regular and serious attempts at celestial navigation. However, the results he obtained were still quite poor, even by the standards of his day.
When he reached the Canary Islands, Columbus split his fleet: three ships would sail west-southwest, direct for Hispaniola, while Columbus himself would take the other three ships southward to the Cape Verde Islands, and then west. The reasons for this maneuver are still debated.
On the passage west from Cape Verde, he made a series of observations of the North Star to determine his latitude. According to Columbus, the North Star varied from 5° to 15° above the horizon, depending on the time of the night. Actually, the North Star was about 3.5° from the celestial pole in 1498, so its total movement in altitude should have been seven degrees, not ten. (This 3.5-degree figure was known to navigators of that era trained in celestial techniques. This is evidence that Columbus was still unfamiliar with important details of celestial navigation.)
The island of Trinidad lies close to the coast of Venezuela and is separated from the mainland by two straits, which Columbus named Boca del Sierpe (serpent’s mouth) and Boca del Drago (dragon’s mouth). Columbus tried to measure the distance between these two straits using celestial observations — or at least, he claimed to. Here’s a quote from a letter Columbus wrote to the King of Spain:
“I found that there between these two straits, which, as I have said, face each other in a line from north to south, it is twenty-six leagues from the one to the other, and I cannot be wrong in this because the calculation was made with a quadrant. . . . In that on the south, which I named la boca de la Sierpe, I found that at nightfall I had the pole star at nearly five degrees elevation, and in the other on the north, which I named la Boca del Drago, it was at almost seven.”
In this case, we know both the dates of the observations (between August 1 and August 12, 1498 — the period in which he explored the Gulf of Paria) and the time of day (nightfall, according to Columbus’s own writings). Therefore we can be fairly sure what the true altitude of the North Star must have been.
Giving Columbus every benefit of the doubt, we may assume that he measured the altitude of Polaris on August 1, 1498, at the Boca del Sierpe (10 N, 62 W) at the beginning of nautical twilight — the time when the Sun reaches 6 degrees below the horizon, and bright stars first become visible. This occurred at 2249 UT for that date and location. At that time, Polaris was already 8° 10′ above the horizon and rising — compared to Columbus’s report of less than 5 degrees.
The observation at Boca del Drago could have been made either on August 4 or August 12, but August 4 is the less unfavorable (nautical twilight began at 2248 UT). His anchorage was 10° 43′ N, 61° 53′ W, so Polaris was already 9° 1′ up (and rising), compared to Columbus’s report of less than 7 degrees.
Errors of two or three degrees are rather large for a quadrant; a skilled navigator, at anchor, should be able to manage a degree or less of error. The most likely explanation for these results is that Columbus had already measured the distance along the west coast of Trinidad using dead reckoning, and it came out at 26 leagues of coastline. His letter records this figure, which is about 69 nautical miles. (And indeed, the west coast of Trinidad is about this long, because it takes a big jog to the east on its way north.)
Columbus then may have created fake observations of Polaris to match his already-known distance, using his adopted size of one degree of latitude, which was 56 2/3 miles (or 14 1/6 leagues). In other words, since Columbus knew that the west coast of Trinidad was 26 leagues long, and he also knew that 28 leagues was about two degrees of latitude, he manufactured “observations” of Polaris that differed by about 2 degrees, to match his dead reckoning.
For more examples of Columbus faking celestial observations to match his dead reckoning, see the page on the eclipse longitudes.
5. The Fourth Voyage
Not much of Columbus’s own writing about the fourth voyage survives today. But we do know that while marooned on the north coast of Jamaica, he found his latitude to be 19°, which is within a degree of the correct number. This high accuracy could only have been achieved if Columbus had been using celestial techniques. It also suggests that even late in his life, Columbus continued to be fascinated with the latest navigational methods, and continued to learn.
Return to The Columbus Navigation Homepage.
(9a) May Earth be Revolving around the Sun?
| Index 7.Precession
|Aristarchus of Samos, an early Greek astronomer (about 310 to 230 BC), was the first to suggest that the Earth revolved around the Sun, rather than the other way around. He gave the first estimate of the distance of the Moon (section (8c)), and it was his careful observation of a lunar eclipse–pin-pointing the Sun’s position on the opposite side of the sky–that enabled Hipparchus, 169 years later, to deduce the precession of the equinoxes).
Except for one calculation–an estimate of the distance and size of the Sun–no work of Aristarchus has survived. However, one could guess why he believed that the Sun, not the Earth, was the central body around which the other one revolved. His calculation suggested that the Sun was much bigger than the Earth–a watermelon, compared to a peach–and it seemed unlikely that the larger body would orbit one so much smaller.
Here we will develop a line of reasoning somewhat like the one Aristarchus used (for his actual calculation, see reference at the end). Aristarchus started from an observation of a lunar eclipse (section (8c)). At such a time the Moon moves through the Earth’s shadow, and what Aristarchus saw convinced him that the shadow was about twice as wide as the Moon. Suppose the width of the shadow was also the width of the Earth (actually it is less–see below, also here). Then the diameter of the Moon would be half the Earth’s.
|Aristarchus next tried to observe exactly when half the moon was sunlit. For this to happen, the angle Earth-Moon-Sun (angle EMS in the drawing here) must be exactly 90 degrees.Knowing the Sun’s motion across the sky, Aristarchus could also locate the point P in the sky, on the Moon’s orbit (near the ecliptic), which was exactly 90 degrees from the direction of the Sun as seen from Earth. If the Sun were very, very far away, the half-moon would also be on this line, at a position like M’ (drawn with a different distance scale, for clarity).
Aristarchus estimated, however, that the direction to the half-moon made a small angle a with the direction to P, about 1/30 of a right angle or 3 degrees.
As the drawing shows, the angle ESM (Earth-Sun-Moon) then also equals 3 degrees. If Rs is the Sun’s distance and Rm the Moon’s, a full 360° circle around the Sun at the Earth’s distance has the length of 2pRs (p = 3.14159…). The distance Rm = EM is then about as long as an arc of that circle, covering only 3° or 1/120 of the full circle. It follows that
Rm = 2pRs/120 ~ Rs/19
making the Sun (according to Aristarchus) 19 times more distant than the Moon. Since the two have very nearly the same size in the sky, even though one of them is 19 times more distant, the Sun must also be 19 times larger in diameter than the Moon.
If now the Moon’s diameter is half the size of the Earth’s, the Sun must be 19/2 or nearly 10 times wider than the Earth. The effect described in the figures of section (8c) modifies this argument somewhat (details here), making the Earth 3 times wider than the Moon, not twice. If Aristarchus had observed correctly, that would make the Sun’s diameter 19/3 times–a bit more than 6 times–that the Earth.
Actually, he had not! His method does not really work because in actuality the position of the half-Moon is very close to the line OP. The angle p, far from being 3 degrees, is actually so small that Aristarchus could never have measured it, especially without a telescope. The actual distance to the Sun is about 400 times that of the Moon, not 19 times, and the Sun’s diameter is similarly about 400 times the Moon’s and more than 100 times the Earth’s
But it makes no difference. The main conclusion, that the Sun is vastly bigger than Earth, still holds. Aristarchus could just as well have said that the angle p was at most 3 degrees, in which case the Sun was at least 19 times more distant than the Moon, and its size at least 19/3 times that of Earth. In fact, he did say so–but he also claimed it was less than 43/6 times larger than the Earth (Greeks used simple fractions–they knew nothing about decimals), which was widely off the mark. But it makes no difference: as long as the Sun is much bigger than the Earth, it makes more sense that it, rather than the Earth, is at the center.
Good logic, but few accepted it, not even Hipparchus and Ptolemy. In fact, the opposite argument was made: if the Earth orbited the Sun, it would be on opposite sides of the Sun every 6 months. If that distance was as big as Aristarchus claimed it to be, would not the positions of the stars differ when viewed from two spots so far apart? We now know the answer: the stars are so far from us, that even with the two points 20 times further apart than Aristarchus had claimed, the best telescopes can barely observe the shift of the stars. It took nearly 18 centuries before the ideas of Aristarchus were revived by Copernicus.
In the year 1600, William Gilbert, physician to Britain’s Queen Elizabeth I and the first investigator of magnetism, published De Magnete (“On the Magnet” in Latin, in which the book was written). That book marks the end of medieval thought, built largely on citations of ancient authors, and the start of modern science based on experiments. (For a large website containing two reviews of the book and the history of the Earth’s magnetism from Gilbert to our time, see here.)
Gilbert was a staunch supporter of Copernicus (see section #9c), but it is interesting to note that he still quotes the result of Aristarchus (Gilbert’s “Book 6”, section 2, about 2/3 through the section), writing “The Sun in its greatest eccentricity has a distance of 1142 semi-diameters of the Earth.” Aristarchus estimated the Sun’s distance to be slightly below 20 times that of the Moon, which was at a distance of about 60 Earth radii, and 20×60 = 1200, close to Gilbert’s figure. In 1800 years, no one had checked that result!
The introduction to Gilbert’ book was written by Edward Wright, who used that value to derive the velocity of the Sun, if it were to circle the Earth every 24 hours, arriving at a speed so high that he considered it impossible:
This is the same argument Aristarchus could have made and probably did.
For advanced students:
Note: The actual calculation by Aristarchus was more complex and less transparent. See A. Pannekoek: A History of Astronomy, Interscience, 1961, p. 118-120 and Appendix A.
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