30.2 Nuclear Reactors 979events in the reactor core supply heat to the water contained in the primary(closed) system, which is maintained at high pressure to keep it from boiling. Thiswater also serves as the moderator. The hot water is pumped through a heatexchanger, and the heat is transferred to the water contained in the secondary system.There the hot water is converted to steam, which drives a turbine–generatorto create electric power. Note that the water in the secondary system is isolatedfrom the water in the primary system in order to prevent contamination of the secondarywater and steam by radioactive nuclei from the reactor core.Reactor Safety 1The safety aspects of nuclear power reactors are often sensationalized by themedia and misunderstood by the public. The 1979 near disaster of Three MileIsland in Pennsylvania and the accident at the Chernobyl reactor in the Ukrainerightfully focused attention on reactor safety. Yet the safety record in the UnitedStates is enviable. The records show no fatalities attributed to commercial nuclearpower generation in the history of the United States nuclear industry.Commercial reactors achieve safety through careful design and rigid operatingprocedures. Radiation exposure and the potential health risks associated with suchexposure are controlled by three layers of containment. The fuel and radioactivefission products are contained inside the reactor vessel. Should this vessel rupture,the reactor building acts as a second containment structure to prevent radioactivematerial from contaminating the environment. Finally, the reactor facilities mustbe in a remote location to protect the general public from exposure should radiationescape the reactor building.According to the Oak Ridge National Laboratory Review, “The health risk of livingwithin 8 km (5 miles) of a nuclear reactor for 50 years is no greater than the riskof smoking 1.4 cigarettes, drinking 0.5 liters of wine, traveling 240 km by car, flying9 600 km by jet, or having one chest x-ray in a hospital. Each of these activities isestimated to increase a person’s chances of dying in any given year by one in amillion.”Another potential danger in nuclear reactor operations is the possibility thatthe water flow could be interrupted. Even if the nuclear fission chain reactionwere stopped immediately, residual heat could build up in the reactor to the pointof melting the fuel elements. The molten reactor core would melt its way to thebottom of the reactor vessel and conceivably into the ground below—the socalledChina syndrome. Although it might appear that this deep undergroundburial site would be an ideal safe haven for a radioactive blob, there would be dangerof a steam explosion should the molten mass encounter water. This nonnuclearexplosion could spread radioactive material to the areas surrounding thepower plant. To prevent such an unlikely chain of events, nuclear reactors aredesigned with emergency core cooling systems, requiring no power, that automaticallyflood the reactor with water in the event of a loss of coolant. The emergencycooling water moderates heat build-up in the core, which in turn prevents themelting of the reactor vessel.A continuing concern in nuclear fission reactors is the safe disposal of radioactivematerial when the reactor core is replaced. This waste material contains longlived,highly radioactive isotopes and must be stored for long periods of time insuch a way that there is no chance of environmental contamination. At present,sealing radioactive wastes in waterproof containers and burying them in deep saltmines seems to be the most promising solution.Transportation of reactor fuel and reactor wastes poses additional safety risks.However, neither the waste nor the fuel of nuclear power reactors can be used toconstruct a nuclear bomb.Accidents during transportation of nuclear fuel could expose the public toharmful levels of radiation. The Department of Energy requires stringent crash1 The authors are grateful to Professor Gene Skluzacek of the University of Nebraska at Omaha for rewriting this section.
980 Chapter 30 Nuclear Energy and Elementary Particlestests on all containers used to transport nuclear materials. Container manufacturersmust demonstrate that their containers will not rupture, even in high-speedcollisions.The safety issues associated with nuclear power reactors are complex and oftenemotional. All sources of energy have associated risks. Coal, for example, exposesworkers to health hazards (including radioactive radon) and produces atmosphericpollution (including greenhouse gases). In each case, the risks must beweighed against the benefits and the availability of the energy source.This photograph of the Sun, taken onDecember 19, 1973, during the thirdand final manned Skylab mission,shows one of the most spectacularsolar flares ever recorded, spanningmore than 588 000 km (365 000 mi)across the solar surface. Several activeregions can be seen on the easternside of the disk. The photograph wastaken in the light of ionized heliumby the extreme ultraviolet spectroheliographinstrument of the U.S.Naval Research Laboratory.NASA30.3 NUCLEAR FUSIONFigure 29.4 shows that the binding energy of light nuclei (those having a massnumber lower than 20) is much smaller than the binding energy of heavier nuclei.This suggests a process that is the reverse of fission. When two light nuclei combineto form a heavier nucleus, the process is called nuclear fusion. Because the massof the final nucleus is less than the masses of the original nuclei, there is a loss ofmass, accompanied by a release of energy. Although fusion power plants have notyet been developed, a worldwide effort is under way to harness the energy fromfusion reactions in the laboratory.Fusion in the SunAll stars generate their energy through fusion processes. About 90% of stars,including the Sun, fuse hydrogen, whereas some older stars fuse helium or otherheavier elements. Stars are born in regions of space containing vast clouds of dustand gas. Recent mathematical models of these clouds indicate that star formationis triggered by shock waves passing through a cloud. These shock waves are similarto sonic booms and are produced by events such as the explosion of a nearby star,called a supernova. The shock wave compresses certain regions of the cloud, causingthem to collapse under their own gravity. As the gas falls inward toward thecenter, the atoms gain speed, which causes the temperature of the gas to rise. Twoconditions must be met before fusion reactions in the star can sustain its energyneeds: (1) The temperature must be high enough (about 10 7 K for hydrogen) toallow the kinetic energy of the positively charged hydrogen nuclei to overcometheir mutual Coulomb repulsion as they collide, and (2) the density of nuclei mustbe high enough to ensure a high rate of collision.It’s interesting that temperatures inside stars like the Sun are not sufficient toallow colliding protons to overcome Coulomb repulsion. In a certain percentageof collisions, the nuclei pass through the barrier anyway, an example of quantumtunneling. So a quantum effect is key in making sunshine.When fusion reactions occur at the core of a star, the energy that is liberatedeventually becomes sufficient to prevent further collapse of the star under its owngravity. The star then continues to live out the remainder of its life under a balancebetween the inward force of gravity pulling it toward collapse and the outwardforce due to thermal effects and radiation pressure.The proton–proton cycle is a series of three nuclear reactions that are believedto be the stages in the liberation of energy in the Sun and other stars rich inhydrogen. An overall view of the proton–proton cycle is that four protonscombine to form an alpha particle and two positrons, with the release of 25 MeVof energy in the process.The specific steps in the proton–proton cycle are11 H 1 1 H : 2 1 D e and11 H 2 1 D : 3 2 He [30.3]where D stands for deuterium, the isotope of hydrogen having one proton and one2neutron in the nucleus. (It can also be written as .) The second reaction is1 H
- Page 1 and 2:
Color-enhanced scanning electronmic
- Page 3:
876 Chapter 27 Quantum PhysicsSolve
- Page 6 and 7:
27.2 The Photoelectric Effect and t
- Page 8 and 9:
27.3 X-Rays 881even when black card
- Page 10 and 11:
27.4 Diffraction of X-Rays by Cryst
- Page 12 and 13:
27.5 The Compton Effect 885Exercise
- Page 14 and 15:
27.6 The Dual Nature of Light and M
- Page 16 and 17:
27.6 The Dual Nature of Light and M
- Page 18 and 19:
27.8 The Uncertainty Principle 891w
- Page 20 and 21:
27.8 The Uncertainty Principle 893E
- Page 22 and 23:
27.9 The Scanning Tunneling Microsc
- Page 24 and 25:
Problems 897The probability per uni
- Page 26 and 27:
Problems 89917. When light of wavel
- Page 28 and 29:
Problems 90151.time of 5.00 ms. Fin
- Page 30 and 31:
“Neon lights,” commonly used in
- Page 32 and 33:
28.2 Atomic Spectra 905l(nm) 400 50
- Page 34 and 35:
28.3 The Bohr Theory of Hydrogen 90
- Page 36 and 37:
28.3 Th Bohr Theory of Hydrogen 909
- Page 38 and 39:
28.4 Modification of the Bohr Theor
- Page 40 and 41:
28.6 Quantum Mechanics and the Hydr
- Page 42 and 43:
28.7 The Spin Magnetic Quantum Numb
- Page 44 and 45:
28.9 The Exclusion Principle and th
- Page 46 and 47:
28.9 The Exclusion Principle and th
- Page 48 and 49:
28.11 Atomic Transitions 921electro
- Page 50 and 51:
28.12 Lasers and Holography 923is u
- Page 52 and 53:
28.13 Energy Bands in Solids 925Ene
- Page 54 and 55:
28.13 Energy Bands in Solids 927Ene
- Page 56 and 57: 28.14 Semiconductor Devices 929I (m
- Page 58 and 59: Summary 931(a)Figure 28.32 (a) Jack
- Page 60 and 61: Problems 9335. Is it possible for a
- Page 62 and 63: Problems 935tum number n. (e) Shoul
- Page 64 and 65: Problems 93748. A dimensionless num
- Page 66 and 67: Aerial view of a nuclear power plan
- Page 68 and 69: 29.1 Some Properties of Nuclei 941T
- Page 70 and 71: 29.2 Binding Energy 943130120110100
- Page 72 and 73: 29.3 Radioactivity 94529.3 RADIOACT
- Page 74 and 75: 29.3 Radioactivity 947INTERACTIVE E
- Page 76 and 77: 29.4 The Decay Processes 949Alpha D
- Page 78 and 79: 29.4 The Decay Processes 951Strateg
- Page 80 and 81: 29.4 The Decay Processes 953they we
- Page 82 and 83: 29.6 Nuclear Reactions 955wounds on
- Page 84 and 85: 29.6 Nuclear Reactions 957EXAMPLE 2
- Page 86 and 87: 29.7 Medical Applications of Radiat
- Page 88 and 89: 29.7 Medical Applications of Radiat
- Page 90 and 91: 29.8 Radiation Detectors 963Figure
- Page 92 and 93: Summary 965Photo Researchers, Inc./
- Page 94 and 95: Problems 967CONCEPTUAL QUESTIONS1.
- Page 96 and 97: Problems 96924. A building has beco
- Page 98 and 99: Problems 97157. A by-product of som
- Page 100 and 101: This photo shows scientist MelissaD
- Page 102 and 103: 30.1 Nuclear Fission 975Applying Ph
- Page 104 and 105: 30.2 Nuclear Reactors 977Courtesy o
- Page 108 and 109: 30.3 Nuclear Fusion 981followed by
- Page 110 and 111: 30.3 Nuclear Fusion 983VacuumCurren
- Page 112 and 113: 30.6 Positrons and Other Antipartic
- Page 114 and 115: 30.7 Mesons and the Beginning of Pa
- Page 116 and 117: 30.9 Conservation Laws 989LeptonsLe
- Page 118 and 119: 30.10 Strange Particles and Strange
- Page 120 and 121: 30.12 Quarks 993n pΣ _ Σ 0 Σ + S
- Page 122 and 123: 30.12 Quarks 995charm C 1, its anti
- Page 124 and 125: 30.14 Electroweak Theory and the St
- Page 126 and 127: 30.15 The Cosmic Connection 999prot
- Page 128 and 129: 30.16 Problems and Perspectives 100
- Page 130 and 131: Problems 100330.12 Quarks &30.13 Co
- Page 132 and 133: Problems 1005particles fuse to prod
- Page 134 and 135: Problems 100740. Assume binding ene
- Page 136 and 137: A.1 MATHEMATICAL NOTATIONMany mathe
- Page 138 and 139: A.3 Algebra A.3by 8, we have8x8 32
- Page 140 and 141: A.3 Algebra A.5EXERCISESSolve the f
- Page 142 and 143: A.5 Trigonometry A.7When natural lo
- Page 144 and 145: APPENDIX BAn Abbreviated Table of I
- Page 146 and 147: An Abbreviated Table of Isotopes A.
- Page 148 and 149: An Abbreviated Table of Isotopes A.
- Page 150 and 151: Some Useful Tables A.15TABLE C.3The
- Page 152 and 153: Answers to Quick Quizzes,Odd-Number
- Page 154 and 155: Answers to Quick Quizzes, Odd-Numbe
- Page 156 and 157:
Answers to Quick Quizzes, Odd-Numbe
- Page 158 and 159:
Answers to Quick Quizzes, Odd-Numbe
- Page 160 and 161:
Answers to Quick Quizzes, Odd-Numbe
- Page 162 and 163:
Answers to Quick Quizzes, Odd-Numbe
- Page 164 and 165:
Answers to Quick Quizzes, Odd-Numbe
- Page 166 and 167:
Answers to Quick Quizzes, Odd-Numbe
- Page 168 and 169:
IndexPage numbers followed by “f
- Page 170 and 171:
Current, 568-573, 586direction of,
- Page 172 and 173:
Index I.5Fissionnuclear, 973-976, 9
- Page 174 and 175:
Index I.7Magnetic field(s) (Continu
- Page 176 and 177:
Polarizer, 805-806, 805f, 806-807Po
- Page 178 and 179:
South poleEarth’s geographic, 626
- Page 180 and 181:
CreditsPhotographsThis page constit
- Page 182 and 183:
PEDAGOGICAL USE OF COLORDisplacemen
- Page 184 and 185:
PHYSICAL CONSTANTSQuantity Symbol V