Roentgen, Wilhelm Conrad


Roentgen, Wilhelm Conrad (1845-1923), German physicist, discoverer of X rays, and winner of the first Nobel Prize in physics. Roentgen's discovery of X rays was a momentous advance for physics and medicine and earned him the 1901 Nobel Prize in physics.

Roentgen was born in Lennep, Germany, and grew up in the Netherlands. He earned a mechanical engineering degree at the Federal Institute of Technology in Zürich, Switzerland, in 1868 and a Ph.D. degree in physics at the University of Zürich in 1869. Roentgen worked as a laboratory assistant at the University of Würzburg in Germany from 1868 to 1872 and at the University of Strasbourg in Germany from 1872 to 1874. He began teaching physics in 1874, starting at the University of Strasbourg, then moving to the Agricultural Academy in Hohenheim, Germany, in 1875, and back to Strasbourg in 1876. In 1879 he became a professor of physics at the University of Giessen in Germany, where he remained until 1888, when he became professor of physics and director of the Physical Institute at the University of Würzburg. He accepted a position as professor of physics and director of the Physical Science Institute at the University of Munich in 1899 and taught there until his retirement in 1920.

Roentgen made an accidental discovery November 8, 1895, while investigating emissions from a Crookes tube (a glass vacuum tube with electrodes at either end). The emissions Roentgen was looking for are called cathode rays, composed of high-speed electrons that come off the negative electrode when voltage is applied to the electrodes of a Crookes tube. Cathode rays cause the vacuum tube to glow when the vacuum is strong enough and enough voltage is applied; it was this glow Roentgen was watching when he made his discovery. Cathode rays are weak—they cannot pass through glass (scientists use aluminum windows in a vacuum tube when they want to study cathode rays outside the tube) or an ordinary piece of cardboard—but they do excite barium platinocyanide molecules and cause surfaces painted with barium platinocyanide to glow.

Roentgen was using a Crookes tube without an aluminum window and he had surrounded the tube in black cardboard to better see the tube glow. Therefore, when he noticed a glow coming from a screen painted with barium platinocyanide that was some distance away, he knew cathode rays could not be the cause, because cathode rays could not have gone through either the glass of the tube or the cardboard. Roentgen did more tests to verify that the Crookes tube was the source of the emissions that made the screen glow. He inferred that these emissions were present in all experiments like his, but that he was the first to notice them because no one else had set up conditions like his experiment: a nearby barium platinocyanide-painted screen and an arrangement that suppressed the known emissions.

Roentgen called the newly discovered emissions X rays (x is the symbol for the unknown in mathematics) and worked to document them further. He found a photographic plate in a drawer of a desk in the same room as the Crookes tube and noticed it had been exposed. When he developed it and found an image of a key that had been on the desk top, he realized the X rays had passed easily through the wood of the desk, but to a lesser degree through the metal of the key. Using a barium platinocyanide-treated screen and a Crookes tube, Roentgen produced an image of a lead disk—and the bones of his fingers holding the disk.

His experiments showed that X rays pass through different materials to different degrees. Release of his findings caused worldwide excitement and speculation about X rays, also called Roentgen rays. Medical applications in diagnosis began immediately. The hazard of burns from prolonged exposure soon became evident; the risk of cancer was realized later. X rays came to be used in medical treatment, dental examinations, industrial inspections of metal work, and many other areas.

Astronomy

Astronomy, study of the universe and the celestial bodies, gas, and dust within it. Astronomy includes observations and theories about the solar system, the stars, the galaxies, and the general structure of space. Astronomy also includes cosmology, the study of the universe and its past and future. People who study astronomy are called astronomers, and they use a wide variety of methods to perform their research. These methods usually involve ideas of physics, so most astronomers are also astrophysicists, and the terms astronomer and astrophysicist are basically identical. Some areas of astronomy also use techniques of chemistry, geology, and biology.

Professional astronomers usually have access to powerful telescopes, detectors, and computers. Most work in astronomy includes three parts, or phases. Astronomers first observe astronomical objects by guiding telescopes and instruments to collect the appropriate information. Astronomers then analyze the images and data. After the analysis, they compare their results with existing theories to determine whether their observations match with what theories predict, or whether the theories can be improved. Some astronomers work solely on observation and analysis, and some work solely on developing new theories.

Astronomy is such a broad topic that astronomers specialize in one or more parts of the field. For example, the study of the solar system is a different area of specialization than the study of stars. Astronomers who study our galaxy, the Milky Way, often use techniques different from those used by astronomers who study distant galaxies. Many planetary astronomers, such as scientists who study Mars, may have geology backgrounds and not consider themselves astronomers at all. Solar astronomers use different telescopes than nighttime astronomers use, because the Sun is so bright. Theoretical astronomers may never use telescopes at all. Instead, these astronomers use existing data or sometimes only previous theoretical results to develop and test theories. An increasing field of astronomy is computational astronomy, in which astronomers use computers to simulate astronomical events. Examples of events for which simulations are useful include the formation of the earliest galaxies of the universe or the explosion of a star to make a supernova.

Astronomers learn about astronomical objects by observing the energy they emit. These objects emit energy in the form of electromagnetic radiation. This radiation travels throughout the universe in the form of waves and can range from gamma rays, which have extremely short wavelengths, to visible light, to radio waves, which are very long. The entire range of these different wavelengths makes up the electromagnetic spectrum.

Astronomers gather different wavelengths of electromagnetic radiation depending on the objects that are being studied. The techniques of astronomy are often very different for studying different wavelengths. Conventional telescopes work only for visible light and the parts of the spectrum near visible light, such as the shortest infrared wavelengths and the longest ultraviolet wavelengths. Earth’s atmosphere complicates studies by absorbing many wavelengths of the electromagnetic spectrum. Gamma-ray astronomy, X-ray astronomy, infrared astronomy, ultraviolet astronomy, radio astronomy, visible-light astronomy, cosmic-ray astronomy, gravitational-wave astronomy, and neutrino astronomy all use different instruments and techniques.

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See also Planetary Science

Planetary Science


Planetary Science, study of the forces and influences that determine the composition, structure, and evolution of planets and planetary systems. Planetary scientists also study how planetary systems form around other stars. In particular, planetary science is a study of the properties of the Earth compared to the properties of other worlds, which helps explain some of the properties of Earth through the example of other planets.

The origins of modern planetary science can be traced to the Copernican revolution of the 16th and 17th centuries, which led to overturning the old idea that Earth is unique and central in creation. Polish astronomer Nicolaus Copernicus, Italian astronomer and philosopher Galileo, and others showed that the Sun is the central body in Earth’s solar system and that Earth is only one planet among several that orbit the Sun. Continued advances in astronomy have revealed that the Sun is an average star in a universe filled with billions of stars. Recent observations indicate that a significant fraction of the stars in the universe could be encircled by planetary systems—some of which may be similar to Earth’s solar system, and many that are probably quite different.

Modern planetary science draws from many fields of science, including astronomy, physics, chemistry, atmospheric science, and geology. To some degree, the study of planets also requires a biological perspective, for it is now clear that the evolution of the atmosphere and surface environment of at least one planet—Earth—has been radically influenced by the presence of life. Many scientists believe that life may not be limited Earth and may, in fact, be fairly common throughout the universe (see Exobiology). Planetary science is therefore also concerned with life on other planets.

Rutherford, Ernest

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Rutherford, Ernest, 1st Baron Rutherford of Nelson and Cambridge (1871-1937), British physicist, who became a Nobel laureate for his pioneering work in nuclear physics and for his theory of the structure of the atom.

Rutherford was born in Nelson, New Zealand, and educated at the University of New Zealand and the University of Cambridge. He was professor of physics at McGill University in Montréal, Québec, Canada, from 1898 to 1907 and at the University of Manchester in England during the following 12 years. After 1919 he was professor of experimental physics and director of the Cavendish Laboratory at the University of Cambridge and also held a professorship, after 1920, at the Royal Institution of Great Britain in London.

Rutherford was one of the first and most important researchers in nuclear physics. Soon after the discovery of radioactivity in 1896 by the French physicist Antoine Henri Becquerel, Rutherford identified the three main components of radiation and named them alpha, beta, and gamma rays. He also showed that alpha particles are helium nuclei. His study of radiation led to his formulation of a theory of atomic structure, which was the first to describe the atom as a dense nucleus about which electrons circulate in orbits.

In 1919 Rutherford conducted an important experiment in nuclear physics when he bombarded nitrogen gas with alpha particles and obtained atoms of an oxygen isotope and protons. This transmutation of nitrogen into oxygen was the first artificially induced nuclear reaction. It inspired the intensive research of later scientists on other nuclear transformations and on the nature and properties of radiation. Rutherford and the British physicist Frederick Soddy developed the explanation of radioactivity that scientists accept today. The rutherford, a unit of radioactivity, was named in his honor.

Galileo

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Galileo (1564-1642), Italian physicist and astronomer, who, with the German astronomer Johannes Kepler, initiated the scientific revolution that flowered in the work of the English physicist Sir Isaac Newton. Born Galileo Galilei, his main contributions were, in astronomy, the use of the telescope in observation and the discovery of sunspots, lunar mountains and valleys, the four largest satellites of Jupiter, and the phases of Venus. In physics, he discovered the laws of falling bodies and the motions of projectiles. In the history of culture, Galileo stands as a symbol of the battle against authority for freedom of inquiry.

Galileo was born near Pisa, on February 15, 1564. His father, Vincenzo Galilei, played an important role in the musical revolution from medieval polyphony to harmonic modulation. Just as Vincenzo saw that rigid theory stifled new forms in music, so his eldest son came to see Aristotelian physical theology as limiting scientific inquiry. Galileo was taught by monks at Vallombrosa and then entered the University of Pisa in 1581 to study medicine. He soon turned to philosophy and mathematics, leaving the university without a degree in 1585. For a time he tutored privately and wrote on hydrostatics and natural motions, but he did not publish. In 1589 he became professor of mathematics at Pisa, where he is reported to have shown his students the error of Aristotle’s belief that speed of fall is proportional to weight, by dropping two objects of different weight simultaneously from the Leaning Tower. His contract was not renewed in 1592, probably because he contradicted Aristotelian professors. The same year, he was appointed to the chair of mathematics at the University of Padua, where he remained until 1610.

At Padua, Galileo invented a calculating “compass” for the practical solution of mathematical problems. He turned from speculative physics to careful measurements, discovered the law of falling bodies and of the parabolic path of projectiles, studied the motions of pendulums, and investigated mechanics and the strength of materials. He showed little interest in astronomy, although beginning in 1595 he preferred the Copernican theory—that the earth revolves around the sun—to the Aristotelian and Ptolemaic assumption that planets circle a fixed earth. Only the Copernican model supported Galileo’s tide theory, which was based on motions of the earth. In 1609 he heard that a spyglass had been invented in Holland. In August of that year he presented a telescope, about as powerful as a modern field glass, to the doge of Venice. Its value for naval and maritime operations resulted in the doubling of his salary and his assurance of lifelong tenure as a professor.