Atomic Secrets The street lamps, the building lights, and the car headlights were photographed with a diffraction grating over the camera lens. Why are the images of the lights different, and how could these differences be used to identify the types of lights?
➥ Look at the text on page 649 for the answer. CHAPTER 28 The Atom
ou have seen that both prisms and diffraction gratings WHAT YOU’LL LEARN separate light into its component colors. But do all sources • You will examine the compo- Y of light produce the same spectrum, that is, the same mix of sition of the atom. colors? Look at the light sources in the photograph at the left— • You will determine specific headlights, street lamps, and building lights. The spectra of these energies of electrons. light sources were produced by placing a diffraction grating over • You will explore the proba- the camera lens. Note the differences among the spectra. Some bility of finding the electrons spectra include every color; in others, there are brighter bands at at specific locations or with specific colors. specific momenta. For more than 100 years, researchers have studied spectra such • You will study lasers. as these to identify sources of light. Because the light sources are made up of different materials, scientists concluded that different atoms produce different spectra. This relationship between chemical WHY IT’S IMPORTANT The quantum model of the composition and spectra has been helpful in astronomy. Because • atom and the transition of analyzing the spectrum of the light produced by an unknown electrons between orbitals material can reveal its chemical makeup, this process has been are responsible for the ability used to determine the array of atoms present in the sun and in to produce artificial lighting, distant stars. In fact, astronomers can even use the spectra of stars determine the composition of to determine the surface temperature of a star. materials, operate electronic Today scientists use spectral analysis to identify and charac- equipment, and produce terize matter. Spectral analysis also helps delineate impurities in special effects for movies. manufactured items such as molten iron or glass. When the study of spectra began, the structure of atoms was unknown. However, the study of the spectrum produced by the simplest atom—hydrogen—led to the discovery of the structure PHYSICS of not only hydrogen, but also of all other atoms. To find out more about the atom, visit the Glencoe Science Web site at science.glencoe.com
645 The Bohr Model 28.1 of the Atom
y the end of the 19th century, most scientists Bagreed that atoms exist. Furthermore, as a OBJECTIVES result of the discovery of the electron by J. J. Thomson, they agreed that • Explain the structure of the atom could not be an indivisible particle. All of the atoms that Thomson the atom. tested contained electrons that had a negative charge. Yet atoms were known to be electrically neutral and much more massive than electrons. • Distinguish continuous spectra from line spectra. Therefore it followed that atoms must contain not only electrons, but mas- sive, positively charged parts as well. • Contrast emission and absorption spectra. The Nuclear Model • Solve problems using the orbital radius and energy- Discovering the nature of the massive part of the atom and the level equations. arrangement of the electrons was a major challenge. Physicists and chemists from many countries both cooperated and competed in searching for the solution to this puzzle. The result provided not only knowledge of the structure of the atom, but also a totally new approach to both physics and chemistry. The history of this work is one of the most exciting stories of the twentieth century. J. J. Thomson believed that a massive, positively charged substance filled the atom. He pictured the electrons arranged within this substance like raisins in a muffin. However, Ernest Rutherford, who was working in England at the same time, performed a series of brilliant experiments F.Y.I. showing that the atom had a very different structure. J. J. Thomson, the discoverer Compounds containing uranium had been found to emit penetrat- of the electron, first called ing rays. Some of these emissions were found to be massive, positively these subatomic particles charged particles moving at high speed. These were later named alpha “corpuscles.” ( ) particles. The particles could be detected by a screen coated with zinc sulfide that emitted a small flash of light, or scintillation, each time an particle hit it, as shown in Figure 28–1.
Source of α particles
Beam of α particles Deflected particles
FIGURE 28–1 After bombarding metal foil with alpha particles, Circular fluorescent screen Rutherford’s team concluded that most of the mass of the atom was concentrated in the nucleus. Gold foil
646 The Atom FIGURE 28–2 Most of the alpha particles that Rutherford directed Gold foil at a thin sheet of gold foil went through it without deflection. A few, however, were deflected at Alpha large angles. particles
Rutherford directed a beam of particles at a thin sheet of gold foil only a few atoms thick. He observed that while most of the particles passed through the sheet, the beam was spread slightly by the foil. Detailed studies of the deflection of particles showed that a few of the particles were deflected at large angles, even larger than 90°. A diagram of this is shown in Figure 28–2. Rutherford was amazed. He had assumed that the mass was spread more or less evenly throughout the atom. He compared his amazement to that of firing a 15-inch cannon shell at tissue paper and then having the shell bounce back and hit him. Using Coulomb’s force law and Newton’s laws of motion, Rutherford concluded that the results could be explained only if all the positive charge of the atom were concentrated in a tiny, massive central core, now called the nucleus. Rutherford’s model is therefore called the nuclear model of the atom. All the positive charge and more than 99.9 percent of the mass of the atom are in its nucleus. Electrons are outside and far away from the nucleus, and they do not contribute a significant amount of mass. The diameter of the atom is 10 000 times larger than the diameter of the nucleus; thus, the atom is mostly empty space. This discovery accounted for the previous observations that almost all of the particles had passed through the gold foil, and that some of the par- ticles had been deflected at large angles.
Atomic spectra How are the electrons arranged around the nucleus of the atom? One of the clues scientists used to answer this question came from studying the light emitted by atoms. The set of light wave- lengths emitted by an atom is called the atom’s emission spectrum. Atoms of gases can be made to emit their characteristic colors by using a gas discharge tube apparatus. A glass tube containing a gas at low pres- sure has metal electrodes at each end. When a high voltage of electricity is applied across the tube, electrons pass through the gas. The electrons FIGURE 28–3 In a gas dis- collide with the gas atoms, transferring energy to them. The atoms then charge tube apparatus, mercury give up this extra energy, emitting it in the form of light. The light emit- gas glows when high voltage ted by mercury is shown in Figure 28–3. is applied.
28.1 The Bohr Model of the Atom 647 y Gas-discharge tube containing gas
High voltage
Detector
Aligning slits Prism a x
The emission spectrum of an atom can be seen by looking at the light through a prism or a diffraction grating or by putting such a grating in front of a camera lens, as was done in the opening photo. The spectrum can be studied in greater detail using the instrument diagrammed in Figure 28–4a and pictured in Figure 28–4b. In this spectroscope, the b light passes through a slit and is then dispersed as it travels through a prism or diffraction grating. A lens system collects the dispersed light for viewing through a telescope or for recording on a photographic plate. c Each wavelength of light forms an image of the slit at different positions. The spectrum of an incandescent solid is a continuous band of colors from red through violet. The spectrum of a gas, however, is a series of d lines of different colors. Each line corresponds to a particular wavelength FIGURE 28–4 A prism spectro- scope can be used to observe of light emitted by the atoms of the gas. Suppose an unidentified gas, emission spectra (a, b). The perhaps neon or hydrogen, is contained in a tube. When it is excited, the emission spectra of neon (c) and gas will emit light at wavelengths characteristic of the atoms of that gas. molecular hydrogen (d) show Thus, the gas can be identified by comparing its wavelengths with the characteristic lines. lines present in the spectrum of a known sample. The emission spectra for neon and hydrogen are shown in Figure 28–4c, and d, respectively. How can the differences in these emissions be used to identify the atoms involved? When the emission spectrum of a combination of ele- ments is photographed, analysis of the lines on the photograph can indicate the identities and the relative concentrations of the elements present. If the material being examined contains a large amount of any particular element, the lines for that element are more intense on the photograph. Through comparison of the intensities of the lines, the per- FIGURE 28–5 This apparatus is centage composition of the material can be determined. Thus, an emis- used to produce the absorption spectrum of sodium. sion spectrum is a useful analytic tool.
White Continuous Projector light Prism spectrum
Sodium vapor Dark lines
648 The Atom FIGURE 28–6 The emission spectrum (a) and the absorption spectrum (b) of sodium are a pictured.
b A gas that is cool and does not emit light will absorb light at charac- Atomic Secrets teristic wavelengths. This set of wavelengths is called an absorption spectrum. To obtain an absorption spectrum, white light is sent ➥ Answers question from through a sample of gas and then through a spectroscope, as shown in page 644. Figure 28–5. The normally continuous spectrum of the white light then has dark lines in it. These lines show that light of some wavelengths has been absorbed. Often, the bright lines of the emission spectrum and the dark lines of the absorption spectrum of a gas occur at the same wave- lengths. Thus, cool gaseous elements absorb the same wavelengths that they emit when excited, as shown in Figure 28–6 for the emission spec- trum and the absorption spectrum of sodium. Analysis of the wave- lengths of the dark lines in an absorption spectrum also can be used to indicate the composition of the gas. In 1814, while examining the spectrum of sunlight, Josef von Fraunhofer noticed some dark lines. These dark lines, now called Fraunhofer lines, are shown in Figure 28–7. To account for these lines, Fraunhofer assumed that the sun has a relatively cool atmosphere of gaseous elements. He reasoned that as light leaves the sun, it passes through these gases, which absorb light at their characteristic wave- lengths. As a result, these wavelengths are missing from the sun’s absorption spectrum. Through a comparison of the missing lines with the known lines of the various elements, the composition of the atmos- phere of the sun was determined. In this manner, the element helium ASTRONOMY was discovered in the sun before it was found on Earth. Spectrographic analysis also has made it possible to determine the composition of stars. CONNECTION Both emission and absorption spectra are valuable scientific tools. As a result of the elements’ characteristic spectra, chemists are able to ana- lyze , identify, and quantify unknown materials by observing the spectra they emit or absorb. The emission and absorption spectra of elements are important in industry as well as in scientific research. For example, steel mills reprocess large quantities of scrap iron of varying composi- tions. The exact composition of a sample of scrap iron can be determined in minutes by spectrographic analysis. The composition of the steel can then be adjusted to suit commercial specifications. Aluminum, zinc, and other metal processing plants employ the same method.
FIGURE 28–7 Fraunhofer lines appear in the absorption spectrum of the sun.
28.1 The Bohr Model of the Atom 649 FIGURE 28–8 The emission spectrum of hydrogen in the
visible range has four lines. 410 nm 434 nm 486 nm 656 nm
The study of spectra is a branch of science known as spectroscopy. Spectroscopists are employed throughout research and industrial communities. Spectroscopy has proven an effective tool to analyze materials on Earth, and it is the only currently available tool to study the composition of stars over the vast expanse of space. The Bohr Model of the Atom In the nineteenth century, many physicists tried to use atomic spectra to determine the structure of the atom. Hydrogen was studied exten- sively because it is the lightest element and has the simplest spectrum. The visible spectrum of hydrogen consists of four lines: red, green, blue, and violet, as shown in Figure 28–8. Any theory that explained the structure of the atom would have to account for these wavelengths, and it would also have to fit Rutherford’s nuclear model. Rutherford had suggested that electrons orbited the nucleus much as the planets orbit the sun. There was, however, a serious problem with this planetary model. An electron in an orbit is constantly accelerated toward the nucleus. As you learned in Chapter 26, electrons that have been accelerated will radi- ate energy by emitting electromagnetic waves. At the rate that an orbiting electron would lose energy, it would spiral into the nucleus in only 10 9 second. But, atoms are known to be stable. Thus, the planetary model was not consistent with the laws of electromagnetism. In addi- tion, if the planetary theory were true, the accelerated electron should radiate energy at all wavelengths. But, as you have seen, the light emitted by atoms is radiated only at specific wavelengths.
FIGURE 28–9 Bohr’s planetary model of the atom postulated that electrons moved in fixed orbits around the nucleus.
650 The Atom Danish physicist Niels Bohr went to England in 1911 and soon joined Rutherford’s group to work on determining the structure of the atom. He tried to unite the nuclear model with Einstein’s theory of light. This was a courageous idea, because in 1911 Einstein’s revolutionary theory F.Y.I. of the photoelectric effect had not yet been confirmed by experiments and was not widely accepted. Recall from Chapter 27 that according to The proton was observed Einstein, light and other forms of electromagnetic radiation consist of in 1919 as a particle that is discrete bundles of energy called photons. That is, light seems to act like emitted when the nucleus of an atom is bombarded a stream of tiny particles. by alpha particles. Bohr energy is quantized Bohr started with the planetary arrange- ment of electrons, diagrammed in Figure 28–9, but he made the bold hypothesis that the laws of electromagnetism do not operate inside atoms. He hypothesized that an electron in a stable orbit does not radi- ate energy, even though it is accelerating. If energy was not radiated when electrons were in stable orbits but elements could emit a characteristic energy spectrum, when was the energy radiated? Bohr suggested that light is emitted when the electron’s energy changes, as shown in Figure 28–10. According to Einstein, the energy of a photon of light is represented by the equation E hf hc/ . Bohr reasoned that if the emission spectrum contains only certain wave- lengths, then an electron can emit or absorb only specific amounts of energy. Therefore, the atomic electrons can have only certain amounts of energy. Recall from Chapter 27 that when energy is found only in cer- tain amounts, it is said to be quantized. The quantization of energy in atoms is unlike everyday experience. For example, if the energy of a pendulum were quantized, it could only oscil- late with certain amplitudes, such as 10 cm or 20 cm, but not for exam- ple, 11.3 cm. Electrons in an atom have different quantized amounts of energy that are called energy levels. When an electron has the smallest allowable amount of energy, it is in the lowest energy level, called the ground state. If an electron absorbs energy, it can make a transition to a higher energy level, called an excited state. Atomic electrons usually remain in excited states for only a few billionths of a second before returning to the ground state and emitting energy. The energy of an orbiting electron in an atom is the sum of the kinetic λ λ λ λ 3 energy of the electron and the potential energy resulting from the attrac- 3 > 2 > 1 E tive force between the electron and the nucleus. The energy of an electron 2 λ 1 in an orbit near the nucleus is less than that of an electron in an orbit far- E 1 λ ther away because work must be done to move an electron to orbits farther 2 away from the nucleus. The electrons in excited states have larger orbits and correspondingly higher energies. The model of an atom having a cen- tral nucleus with its electrons occupying specific quantized energy levels is Eground known as the Bohr model of the atom. FIGURE 28–10 The energy of Einstein’s theory holds that the light photon has an energy hf. Bohr pos- the emitted photon is equal to tulated that the change in the energy of an atomic electron when a photon the difference in energy between is absorbed is equal to the energy of that photon. When the electron two energy levels.
28.1 The Bohr Model of the Atom 651 makes the return transition to the ground state, a photon is emitted. The energy of the photon is equal to the energy difference between the excited and ground states as defined by the following relationship.