Galileo and the Church

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Galileo's many observations of the solar system led the famous mathematician and astronomer to conclude that the planets revolved around the sun. However, he was not the first to propose such an idea. In 1514, the Polish mathematician Nicolaus Copernicus published a book titled Little Commentary in which he set forth several principles, which he called axioms, concerning the solar system. One of the axioms stated that Earth was not the center of the universe, and a second argued that all the planets including Earth were in motion around the center of the universe near the sun.

Although Galileo's acceptance of the Copernican view of the solar system was not revolutionary, it nonetheless attracted the attention of the Catholic Church. Church authorities had cited passages from the Bible that they believed indicated that God had made Earth the center of the universe, with all other bodies revolving around it. As word spread about Galileo's contradiction of church doctrine, Pope Urban VIII summoned him to Rome to express his displeasure.

In 1616, Pope Urban ordered Galileo to admit he had erred in supporting the Copernican theory that Earth revolves around the sun. Galileo's refusal to recant created friction between Europe's most famous scientist and the pope. Following years of charges and countercharges, in 1633 Galileo was tried by a church court and found guilty of continuing to promote his theory. He was placed under arrest, yet continued writing while living out the rest of his life under papal confinement.

of mountains and plains pocked with deep craters. Rotating it toward Jupiter he made the discovery that the distant planet had four moons. Of even greater significance, Galileo eventually provided the first primitive mapping of the major stars of Earth's galaxy, the Milky Way. Based on nothing more than brightness, he mapped the largest stars into seven concentric circles that he called "magnitudes." Magnitude 1, the innermost circle, contained the stars nearest to Earth, while magnitude 7 contained those farthest away. When he was done with this huge task, one evening he wrote in his journal:

You will behold through the looker a host of other stars, which escape the unassisted sight, so numerous as to be beyond belief. Stars of the seventh magnitude appear with the aid of the looker larger and brighter than stars of the second magnitude seen with the unassisted sight.2

Galileo named his most recently built looker "Old Discoverer" and commented in letters to his friends that it was his best of more than one hundred previous models. Barely three feet long and containing two magnifying lenses, each one inch in diameter, it was capable of magnifying objects twenty-eight times their actual size. The light from distant stars, he explained, was refracted, or bent, as it struck the two lenses magnifying it. Old Discoverer was therefore an early refracting telescope. The historic instrument is now on display at the Institute and Museum of the History of Science in Florence, Italy.

In March 1610, Galileo published a description of his night sky observations titled Sidereus Nuncius, Latin for The Starry Messenger. This twenty-four-page book excited scientific thinkers with detailed descriptions of the heavens yet unseen by other scientists. Galileo revealed to his readers the distant scatter of night light to be millions upon millions of stars and colorful swirls of what appeared to be dust (which astronomers now know to be dense gases). In a more general and controversial statement, Galileo challenged the Catholic Church's teachings that Earth was the center of the universe. Agreeing with his predecessor Nicolaus Copernicus, Galileo boldly argued that Earth orbited the sun along with the other planets.

Galileo was delighted with his discoveries but disturbed by the sharp criticism he received from the church. Most church leaders believed his observations to be preposterous and blasphemous because they contradicted the church's contention that Earth was the center of the universe—a belief based on the importance of humankind in scripture. Catholic authorities told Galileo that his looker did nothing more than create optical illusions. The church insisted that the images he and other scientists saw could not be trusted.

On the night of April 14, 1611, to demonstrate their support for Galileo's controversial discoveries, scientists outside Rome held a banquet in Galileo's honor. Galileo let them peer through Old Discoverer. An unidentified Greek poet happened to be present who proposed that the refracting looker be given the name telescope, a Greek word meaning "to see into the distance."

Galileo's dispute with theologians was ongoing and placed him in conflict with them for the remainder of his life. Still, Galileo gave telescopes and astronomy the first major scientific boost. The contemporary astronomer N.M. Swerdlow said of Galileo's astronomical discoveries: "In about two months, December and January [1609-1610], he made more discoveries with his telescope that changed the world than anyone has ever made before or since."3 The European astronomers who followed Galileo were eager to improve upon his findings and test the abilities of telescopes to explore the universe more thoroughly.

A Surge of Refracting Telescopes

Following Lippershey and Galileo, the objective of the next generation of telescope builders was twofold: To increase the light-collecting capability of telescopes and to improve their resolution, or sharpness of focus. In order to achieve these objectives, a major problem had to be resolved. Glass lenses, which had to be polished to form a slight concavity or curvature, caused incoming light to refract, or bend, just as a stick inserted halfway in water appears to bend below the surface. The amount of refraction varied depending upon the different wavelengths of entering light. Each wavelength corresponds to a different color; red has the longest wavelength and violet has the shortest. This means that the focus point for each wavelength, or color, lies at a different distance from the lens. As a result, all the light coming down an early telescope

Polish astronomer Hevelius built this telescope that measured 158 feet in length. Although the telescope had great magnifying power, its size made the instrument unwieldy.

tube could not be focused at a single point for the observer's eye. An astronomer looking at a distant object saw the object surrounded by what appeared to be a halo of color similar to a circular rainbow. This distracting phenomenon is known to astronomers as chromatic aberration, although its cause was originally unknown.

What astronomers did know from trial and error was that the easiest way to reduce chromatic aberration was to flatten the lenses while increasing the space between them, called the focal length. With flat-

Polish astronomer Hevelius built this telescope that measured 158 feet in length. Although the telescope had great magnifying power, its size made the instrument unwieldy.

ter lenses, all wavelengths of light would focus better at the eye of the observer, and as the focal length increased, so did magnification.

The last of these two design changes touched off a competition to see who could build the longest refracting telescope. Although the lenses did not grow much in size (about six to eight inches in diameter), the barrel lengthened to enormous proportions. An astronomer by the name of Hevelius of Danzig provided detailed mappings of the moon using a telescope with an astonishing focal length of 158 feet. The problem with such long, narrow, and unwieldy contrivances was twofold. First, transporting the long, narrow tubes was a major feat, and second, once a location was chosen, setting the barrel sections in a perfectly straight line was almost impossible.

In 1663, recognizing that the problem of chromatic aberration was not being completely eliminated by longer and longer refracting telescopes, the Scottish mathematician James Gregory published Optica Promota, in which he described the first practical reflecting telescope (now known as the Gregorian telescope). Rather than using lenses that refract light, his revolutionary contribution was to describe mathematically the capture of light by a mirror that reflected the light to an astronomer's eyepiece. The use of mirrors instead of glass lenses to capture and focus light meant that the tube of the Gregorian telescope could be shorter but of larger diameter than refractor telescopes. Unfortunately, Gregory never built his reflector telescope; that task would fall to the English mathematician Isaac Newton.

Isaac Newton's Innovation

In 1670, Isaac Newton was a young mathematician studying the mathematics and physics of optics at Cambridge University in England. During his research, he reached the conclusion that visible sunlight was not as simple an entity as his predecessors had supposed.

Every scientist since Aristotle had believed that sunlight was a simple, pure phenomenon, but the chromatic aberration in telescope lenses convinced Newton that sunlight required further investigation.

As an experiment to determine whether sunlight was a single entity or something more complicated, Newton made a glass prism and placed it on a table in his Cambridge apartment. He then drilled a small hole in the window shutter and closed the shutter to darken the room except for the single beam of sunlight passing through the tiny hole. He then positioned the prism on the table so that a beam of light would pass through the prism and project on the opposite wall. Newton theorized that if sunlight is a composite of many colors, he would see a smear of color on the wall. As he slid the prism into the path of the ray of light and turned to see the result, his answer appeared in a blaze of individual colors stretched out on the wall.

Dazzled by what he had discovered, Newton received credit for the revolutionary discovery that sunlight is a mixture of many different wavelengths that are refracted at slightly different angles and that each different wavelength produces a different spectral color. Observing the colorful spectrum of light on the wall, Newton correctly concluded that at the far left of the spectrum, red had the longest wavelength, followed by orange, yellow, green, blue, indigo, and, shortest at the far right, violet. Newton recognized that this was the very same arrangement of colors seen in the spectrum of rainbows and in chromatic aberration.

Now knowing that light was refracted into the spectrum, Newton erroneously concluded that telescopes using refracting lenses would always suffer chromatic aberration. He could think of no solution to correct it. As a result, Newton constructed a new type of telescope based on Gregory's Optica Promota that could magnify and focus light by reflecting it rather than refracting it.

Reflection Rather than Refraction

Newton drew up his first design in 1670 but did not receive scientific acclaim for it until he published his ideas more fully in 1700 in his treatise Opticks. What made Newton's telescope unique to seventeenth-century astronomers was his abandonment of a glass lens through which light passed to focus and form an image,

Isaac Newton invented this telescope that magnified and focused light using mirrors. Also pictured is a manuscript page with Newton's drawing of the telescope.

in favor of a concave mirror off of which light reflected to focus and form an image.

Newton, following Gregory's design, demonstrated that a concave mirror focuses all wavelengths of sunlight at the same point, thereby avoiding the troublesome chromatic aberration produced by refracting telescopes. Newton's telescope, now on display at the Royal Society in London, was just 12 inches long with a primary mirror 1.5 inches in diameter. Using mirrors solved the problem of excessively long, unwieldy refracting tubes. In addition, the magnification power of Newton's reflective mirror reached 38, making Newton's instrument decidedly more powerful than Galileo's refracting telescope.

Newton's reflecting telescope worked in an entirely new way. Light from space was collected by the primary concave mirror and then reflected and focused back on a smaller secondary concave mirror. This secondary mirror was inclined at a forty-five-degree angle to the primary mirror to reflect a second time the focused light to an eyepiece on the side of the telescope barrel, where an astronomer could view the image. By all historical accounts, Newton was far more fascinated by the mathematics and mechanics of telescopes than he was by looking through them into space. Few of his letters discuss observations on the night sky, yet hundreds discuss building telescopes and perfecting mirrors. All mirrors at this time were fabricated from a metal alloy consisting of three parts copper, one part tin, and one part arsenic. The arsenic was added to impart the highest reflective coating possible. Hours of shaping and then polishing were required. In 1704, Newton wrote about polishing a primary mirror:

I ground the object metal with a brisk motion for three or four minutes of time with pitch [resin], leaning hard upon it. Then I placed fresh putty [polishing grit] and ground it again until it had done making a noise [grinding sound], and this work I repeated until the metal was polished, grinding it the last time with all my strength and frequently breathing upon the pitch, to keep it moist without laying on any more putty.4

Contemporary optical engineers estimate that Newton's mirrors reflected little more than 15 percent of the light entering the telescope tube. Nonetheless, his telescope design was a monumental and historic improvement over refracting telescopes. His reflecting telescope not only avoided the problem of chromatic aberration but also focused more accurately and was easily transportable. Best of all, it could see more distant objects than Hevelius's cumbersome contraption.

The new reflecting telescope, however, was not without its problems. Having the eyepiece on the side of the barrel was inconvenient for astronomers, and the secondary mirror tilted at its forty-five-degree angle caused some degradation of incoming light. In 1672, the Frenchman Guillaume Cassegrain was reviewing Newton's telescope design and devised a remedy to the tilted secondary mirror and to the side-mounted eyepiece. His solution, which was named after him, continues to be incorporated into the designs of modern reflector telescopes. Cassegrain proposed three significant design changes. First, the secondary mirror should be convex rather than concave. Second, the secondary mirror should be set parallel (face to face) to the primary mirror rather than at a forty-five-degree angle. And third, and most important of all, a small hole should be drilled in the very center of the primary mirror to allow the light ray, as reflected by the secondary mirror, to pass through and reach an astronomer viewing from the tail end of the barrel.

With these revolutionary enhancements, entering light is first captured by the primary mirror and focused back on the smaller secondary mirror, which in turn focuses it back through the small center hole in the primary mirror on its way to the astronomer's eye.

Using this design, there is less degradation of light and the observer can more handily point the telescope in the direction of observation.

Solving the Problem of Chromatic Aberration

Design improvements by Newton and Cassegrain made reflecting telescopes far more valuable to astronomers than refracting telescopes, but they continued to be plagued by poor-quality metal mirrors. Constantly in need of polishing, metal mirrors quickly distorted and corroded. Seventeenth-century astronomers found themselves spending far too much time grinding and polishing instead of stargazing.

Some time during the mid-1730s, amateur astronomers frustrated by metal mirrors attacked the problem of chromatic aberration in spite of Newton's pronouncement that no solution was possible. By experimenting with a variety of different types of glass lenses, the Englishman Chester Moor Hall stumbled on a solution. Being an amateur, he contracted with optician George Bass to make two 2.5-inch lenses, one made of crown glass (exceptionally hard and clear with low refraction) and the other a concave lens of flint glass (soft and heavy with high refraction). When Bass combined the two, he discovered that they eliminated chromatic aberration. This combination of lenses was called an achromatic lens.

Failing to understand the significance of his discovery, Bass neglected to notify Hall. Then, twenty years later, in the mid-1750s, Bass contacted John Dollond about the achromatic lens. John's son, Peter, saw a commercial application for the lens and applied for a patent. When Hall found out about it, he sued in court but lost because, although he had conceived the idea, he had failed to bring it to fruition. By 1780, hundreds of astronomers snapped up Dollond's lenses, mounted them to refracting telescopes only a few feet long, and saw the stars and planets more clearly than ever.

Such an improved refracting telescope did not end the refractor versus reflector debate and competition. What it did resolve, however, as the eighteenth century came to a close, was that telescopes were destined to become larger.

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