TR-12 (1).ppt
- 1. 1 12.1 Discovery of the Neutron 12.2 Nuclear Properties 12.3 The Deuteron 12.4 Nuclear Forces 12.5 Nuclear Stability 12.6 Radioactive Decay 12.7 Alpha, Beta, and Gamma Decay 12.8 Radioactive Nuclides CHAPTER 12 The Atomic Nucleus It is said that Cockroft and Walton were interested in raising the voltage of their equipment, its reliability, and so on, more and more, as so often happens when you are involved with technical problems, and that eventually Rutherford lost patience and said, “If you don’t put a scintillation screen in and look for alpha particles by the end of the week, I’ll sack the lot of you.” And they went and found them (the first nuclear transmutations). - Sir Rudolf Peierls in Nuclear Physics in Retrospect
- 2. 2 12.1: Discovery of the Neutron Rutherford proposed the atomic structure with the massive nucleus in 1911. Scientists knew which particles compose the nucleus in 1932. Reasons why electrons cannot exist within the nucleus: 1) Nuclear size The uncertainty principle puts a lower limit on its kinetic energy that is much larger that any kinetic energy observed for an electron emitted from nuclei. 2) Nuclear spin If a deuteron consists of protons and electrons, the deuteron must contain 2 protons and 1 electron. A nucleus composed of 3 fermions must result in a half-integral spin. But it has been measured to be 1.
- 3. 3 Discovery of the Neutron 3) Nuclear magnetic moment: The magnetic moment of an electron is over 1000 times larger than that of a proton. The measured nuclear magnetic moments are on the same order of magnitude as the proton’s, so an electron is not a part of the nucleus. In 1930 the German physicists Bothe and Becker used a radioactive polonium source that emitted α particles. When these α particles bombarded beryllium, the radiation penetrated several centimeters of lead.
- 4. 4 Discovery of the Neutron The electromagnetic radiation (photons) are called gamma rays which have energies on the order of MeV. Curie and Joliot performed several measurements to study penetrating high-energy gamma rays. In 1932 Chadwick proposed that the new radiation produced by α + Be consisted of neutrons. His experimental data estimated the neutron’s mass as somewhere between 1.005 u and 1.008 u, not far from the modern value of 1.0087 u.
- 5. 5 12.2: Nuclear Properties The nuclear charge is +e times the number (Z) of protons. Hydrogen’s isotopes: Deuterium: Heavy hydrogen. Has a neutron as well as a proton in its nucleus. Tritium: Has two neutrons and one proton. The nuclei of the deuterium and tritium atoms are called deuterons and tritons. Atoms with the same Z, but different mass number A, are called isotopes.
- 6. 6 Nuclear Properties The symbol of an atomic nucleus is . where Z = atomic number (number of protons) N = neutron number (number of neutrons) A = mass number (Z + N) X = chemical element symbol Each nuclear species with a given Z and A is called a nuclide. Z characterizes a chemical element. The dependence of the chemical properties on N is negligible. Nuclides with the same neutron number are called isotones and the same value of A are called isobars.
- 7. 7 Atomic masses are denoted by the symbol u. 1 u = 1.66054 × 10−27 kg = 931.49 MeV/c2 Both neutrons and protons, collectively called nucleons, are constructed of other particles called quarks. Nuclear Properties
- 8. 8 Sizes and Shapes of Nuclei Rutherford concluded that the range of the nuclear force must be less than about 10−14 m. Assume that nuclei are spheres of radius R. Particles (electrons, protons, neutrons, and alphas) scatter when projected close to the nucleus. It is not obvious whether the maximum interaction distance refers to the nuclear size (matter radius), or whether the nuclear force extends beyond the nuclear matter (force radius). The nuclear force is often called the strong force. Nuclear force radius ≈ mass radius ≈ charge radius
- 9. 9 Sizes and Shapes of Nuclei The nuclear radius may be approximated to be R = r0A1/3 where r0 ≈ 1.2 × 10−15 m. We use the femtometer with 1 fm = 10−15 m, or the fermi. The lightest nuclei by the Fermi distribution for the nuclear charge density ρ(r) is
- 10. 10 Sizes and Shapes of Nuclei If we approximate the nuclear shape as a sphere, The nuclear mass density is 2.3 × 1017 kg / m3. The shape of the Fermi distribution
- 11. 11 The proton’s intrinsic magnetic moment points in the same direction as its intrinsic spin angular momentum. Nuclear magnetic moments are measured in units of the nuclear magneton μN. The divisor in calculating μN is the proton mass mp, which makes the nuclear magneton some 1800 times smaller than the Bohr magneton. The proton magnetic moment is μp = 2.79μN. The magnetic moment of the electron is μe = −1.00116μB. The neutron magnetic moment is μn = −1.91μN. The nonzero neutron magnetic moment implies that the neutron has negative and positive internal charge components at different radii. Complex internal charge distribution. Intrinsic Magnetic Moment
- 12. 12 12.3: The Deuteron The determination of how the neutron and proton are bound together in a deuteron. The deuteron mass = 2.013553 u. The mass of a deuteron atom = 2.014102 u. The difference = 0.000549 u. the mass of an electron. The deuteron nucleus is bound by a mass-energy Bd. The mass of a deuteron is Add an electron mass to each side of Eq. (12.6)
- 13. 13 The Deuteron md + me is the atomic deuterium mass M(2H) and mp + me is the atomic hydrogen mass. Thus Eq.(12.7) becomes Because the electron masses cancel in almost all nuclear-mass difference calculations, we use atomic masses rather than nuclear masses. Convert this to energy using u = 931.5 MeV / c2. Even for heavier nuclei we neglect the electron binding energies (13.6 eV) because the nuclear binding energy (2.2 MeV) is almost one million times greater.
- 14. 14 The Deuteron The binding energy of any nucleus = the energy required to separate the nucleus into free neutrons and protons. Experimental Determination of Nuclear Binding Energies Check the 2.22-MeV binding energy by using a nuclear reaction. We scatter gamma rays from deuteron gas and look for the breakup of a deuteron into a neutron and a proton: This nuclear reaction is called photodisintegration or a photonuclear reaction. The mass-energy relation is where hf is the incident photon energy. Kn and Kp are the neutron and proton kinetic energies.
- 15. 15 The Deuteron The minimum energy required for the photodisintegration: Momentum must be conserved in the reaction (Kn, Kp ≠ 0). Experiment shows that a photon of energy less than 2.22 MeV cannot dissociate a deuteron. Deuteron Spin and Magnetic Moment Deuteron’s nuclear spin quantum number is 1. This indicates the neutron and proton spins are aligned parallel to each other. The nuclear magnetic moment of a deuteron is 0.86μN ≈ the sum of the free proton and neutron 2.79μN − 1.91μN = 0.88μN.
- 16. 16 12.4: Nuclear Forces The angular distribution of neutron classically scattered by protons. Neutron + proton (np) and proton + proton (pp) elastic. The nuclear potential
- 17. 17 Nuclear Forces The internucleon potential has a “hard core” that prevents the nucleons from approaching each other closer than about 0.4 fm. The proton has charge radius up to 1 fm. Two nucleons within about 2 fm of each other feel an attractive force. The nuclear force (short range): It falls to zero so abruptly with interparticle separation. stable. The interior nucleons are completely surrounded by other nucleons with which they interact. The only difference between the np and pp potentials is the Coulomb potential shown for r ≥ 3 fm for the pp force.
- 18. 18 Nuclear Forces The nuclear force is known to be spin dependent. The neutron and proton spins are aligned for the bound state of the deuteron, but there is no bound state with the spins antialigned. The nn system is more difficult to study because free neutrons are not stable from analyses of experiments. The nuclear potential between two nucleons seems independent of their charge (charge independence of nuclear forces). The term nucleon refers to either neutrons or protons because the neutron and proton can be considered different charge states of the same particle.
- 19. 19 12.5: Nuclear Stability The binding energy of a nucleus against dissociation into any other possible combination of nucleons. Ex. nuclei R and S. Proton (or neutron) separation energy: The energy required to remove one proton (or neutron) from a nuclide. All stable and unstable nuclei that are long-lived enough to be observed.
- 20. 20 Nuclear Stability The line representing the stable nuclides is the line of stability. It appears that for A ≤ 40, nature prefers the number of protons and neutrons in the nucleus to be about the same Z ≈ N. However, for A ≥ 40, there is a decided preference for N > Z because the nuclear force is independent of whether the particles are nn, np, or pp. As the number of protons increases, the Coulomb force between all the protons becomes stronger until it eventually affects the binding significantly. The work required to bring the charge inside the sphere from infinity is
- 21. 21 Nuclear Stability For a single proton, The total Coulomb repulsion energy in a nucleus is For heavy nuclei, the nucleus will have a preference for fewer protons than neutrons because of the large Coulomb repulsion energy. Most stable nuclides have both even Z and even N (even-even nuclides). Only four stable nuclides have odd Z and odd N (odd-odd nuclides).
- 22. 22 The Liquid Drop Model Treats the nucleus as a collection of interacting particles in a liquid drop. The total binding energy, the semi-empirical mass formula is The volume term (av) indicates that the binding energy is approximately the sum of all the interactions between the nucleons. The second term is called the surface effect because the nucleons on the nuclear surface are not completely surrounded by other nucleons. The third term is the Coulomb energy in Eq. (12.17) and Eq. (12.18).
- 23. 23 The Liquid Drop Model The fourth term is due to the symmetry energy. In the absence of Coulomb forces, the nucleus prefers to have N ≈ Z and has a quantum- mechanical origin, depending on the exclusion principle. The last term is due to the pairing energy and reflects the fact that the nucleus is more stable for even-even nuclides. Use values given by Fermi to determine this term. where Δ = 33 MeV·A−3/4. No nuclide heavier than has been found in nature. If they ever existed, they must have decayed so quickly that quantities sufficient to measure no longer exist.
- 24. 24 Binding Energy Per Nucleon Use this to compare the relative stability of different nuclides. It peaks near A = 56. The curve increases rapidly, demonstrating the saturation effect of nuclear force. Sharp peaks for the even-even nuclides 4He, 12C, and 16O tight bound.
- 25. 25 Nuclear Models Current research focuses on the constituent quarks and physicists have relied on a multitude of models to explain nuclear force behavior. 1) Independent-particle models: The nucleons move nearly independently in a common nuclear potential. The shell model has been the most successful of these. 2) Strong-interaction models: The nucleons are strongly coupled together. The liquid drop model has been successful in explaining nuclear masses as well as nuclear fission.
- 26. 26 Nuclear Models The difference of the shape between the proton and the neutron are due to the Coulomb interaction on the proton. Nuclei have a Fermi energy level which is the highest energy level filled in the nucleus. In the ground state of a nucleus, all the energy levels below the Fermi level are filled. The nuclear potential felt by the neutron and the proton
- 27. 27 Nuclear Models Energy-level diagrams for 12C and 16O. Both are stable because they are even-even. Case 1: If we add one proton to 12C to make unstable Case 2: If we add one neutron to 12C to make 13C: stable
- 28. 28 Nuclear Models Even when we add another neutron to produce 14C, we find it is barely unstable. Indicating neutron energy levels to be lower in energy than the corresponding proton ones. In this mass region, nature prefers the number of neutrons and protons to be N ≈ Z, but it doesn’t want N ≈ Z. This helps explain why 13C is stable, but not 13N.
- 29. 29 12.6: Radioactive Decay Marie Curie and her husband Pierre discovered polonium and radium in 1898. The simplest decay form is that of a gamma ray, which represents the nucleus changing from an excited state to lower energy state. Other modes of decay include emission of α particles, β particles, protons, neutrons, and fission. The disintegrations or decays per unit time (activity). where dN / dt is negative because total number N decreases with time.
- 30. 30 Radioactive Decay SI unit of activity is the becquerel: 1 Bq = 1 decay / s. Recent use is the Curie (Ci) 3.7 × 1010 decays / s. If N(t) is the number of radioactive nuclei in a sample at time t, and λ (decay constant) is the probability per unit time that any given nucleus will decay: If we let N(t = 0) ≡ N0 ----- radioactive decay law
- 31. 31 Radioactive Decay The activity R is where R0 is the initial activity at t = 0. It is common to refer to the half-life t1/2 or the mean lifetime τ rather than its decay constant. The half-life is The mean lifetime is
- 32. 32 Radioactive Decay The number of radioactive nuclei as a function of time
- 33. 33 When a nucleus decays, all the conservation laws must be observed: Mass-energy Linear momentum Angular momentum Electric charge Conservation of nucleons The total number of nucleons (A, the mass number) must be conserved in a low-energy nuclear reaction or decay. 12.7: Alpha, Beta, and Gamma Decay
- 34. 34 Alpha, Beta, and Gamma Decay Let the radioactive nucleus be called the parent and have the mass Two or more products can be produced in the decay. Let the lighter one be My and the mass of the heavier one (daughter) be MD. The conservation of energy is where Q is the energy released (disintegration energy) and equal to the total kinetic energy of the reaction products. If B > 0, a nuclide is bound and stable; If Q > 0, a nuclide is unbound, unstable, and may decay. If Q < 0, decay emitting nucleons do not occur.
- 35. 35 Alpha Decay The nucleus 4He has a binding energy of 28.3 MeV. If the last two protons and two neutrons in a nucleus are bound by less than 28.3 MeV, then the emission of an alpha particle (alpha decay) is possible. If Q > 0, alpha decay is possible. EX. The appropriate masses are
- 36. 36 Alpha Decay Insert into Eq.(12.31) In order for alpha decay to occur, two neutrons and two protons group together within the nucleus prior to decay and the alpha particle has difficulty in overcoming the nuclear attraction from the remaining nucleons to escape. The potential energy diagram of alpha particle
- 37. 37 Alpha Decay The barrier height VB is greater than 20 MeV. The kinetic energies of alpha particles emitted from nuclei range from 4-10 MeV. It is impossible classically for the alpha particle to reach the nucleus, but the alpha particles are able to tunnel through the barrier. A higher energy E2 has much higher probability than does a lower energy E1. There is a correlation between lower energies and greater difficulty of escaping (longer lifetimes).
- 38. 38 Alpha Decay Assume the parent nucleus is initially at rest so that the total momentum is zero. The final momenta of the daughter pD and alpha particle pα have the same magnitude and opposite directions.
- 39. 39 Alpha Decay From the conservation of energy and conservation of linear momentum, determine a unique energy for the alpha particle.
- 40. 40 Beta Decay Unstable nuclei may move closer to the line of stability by undergoing beta decay. The decay of a free neutron is The beta decay of 14C (unstable) to form 14N, a stable nucleus, can be written as The electron energy spectrum from the beta decay
- 41. 41 Beta Decay There was a problem in neutron decay, the spin ½ neutron cannot decay to two spin ½ particles, a proton and an electron. 14C has spin 0, 14N has spin 1, and the electron has spin ½. we cannot combine spin ½ & 1 to obtain a spin 0. Wolfgang Pauli suggested a neutrino that must be produced in beta decay. It has spin quantum number ½, charge 0, and carries away the additional energy missing in Fig. (12.14).
- 42. 42 Beta Decay An occasional electron is detected with the kinetic energy Kmax required to conserve energy, but in most cases the electron’s kinetic energy is less than Kmax. the neutrino has little or no mass, and its energy may be all kinetic. Neutrinos have no charge and do not interact electromagnetically. They are not affected by the strong force of the nucleus. They are the weak interaction. The electromagnetic and weak forces are the electroweak force.
- 43. 43 β- Decay There are antineutrinos . The beta decay of a free neutron of 14C is written as In the general beta decay of the parent nuclide to the daughter , the reaction is The disintegration energy Q is In order for β− to occur, we must have Q > 0. The nucleus A is constant, but Z charges to Z + 1.
- 44. 44 β+ Decay What happens for unstable nuclides with too many protons? Positive electron (positron) is produced. Positron is the antiparticle of the electron. A free proton does not decay when t1/2 > 1032 y. The nucleus 14O is unstable and decays by emitting a positron to become stable 14N. The general β+ decay is The disintegration energy Q is
- 45. 45 Electron Capture Classically, inner K-shell and L-shell electrons are tightly bound and their orbits are highly elliptical, these electrons spend a time passing through the nucleus, thereby the possibility of atomic electron capture. The reaction for a proton is p + e− → n + v The general reaction is The disintegration energy Q is
- 46. 46 Gamma Decay If the decay proceeds to an excited state of energy Ex rather than to the ground state, then Q for the transition to the excited state can be determined with respect to the transition to the ground state. The disintegration energy Q to the ground state Q0. Q for a transition to the excited state Ex is
- 47. 47 Gamma Decay The excitation energies tend to be much larger, many keV or even MeV. The possibilities for the nucleus to rid itself of this extra energy is to emit a photon (gamma ray). The gamma-ray energy hf is given by the difference of the higher energy state E> and lower one E<. The decay of an excited state of AX* (where * is an excited state) to its ground state is A transition between two nuclear excited states E> and E< is
- 48. 48 Gamma Decay The gamma rays are normally emitted soon after the nucleus is created in an excited state. Sometimes selection rules prohibit a certain transition, and the excited state may live for a long time. These states are called isomers or isomeric states and are denoted by a small m for metastable. Ex: the spin 9 state of at 0.271 MeV excitation energy does not gamma decay because of a large spin difference transition. Even though is another example of prohibited (the probability of occurring is small) decay to the ground state, it does gamma decay.
- 49. 49 12.8: Radioactive Nuclides The unstable nuclei found in nature exhibit natural radioactivity.
- 50. 50 Radioactive Nuclides The radioactive nuclides made in the laboratory exhibit artificial radioactivity. Heavy radioactive nuclides can change their mass number only by alpha decay (AX → A−4D) but can change their charge number Z by either alpha or beta decay. There are only four paths that the heavy naturally occurring radioactive nuclides may take as they decay. Mass numbers expressed by either: 4n 4n + 1 4n + 2 4n + 3
- 51. 51 Radioactive Nuclides The sequence of one of the radioactive series 232Th 212Bi can decay by either alpha or beta decay (branching).
- 52. 52 Time Dating Using Lead Isotopes A plot of the abundance ratio of 206Pb / 204Pb versus 207Pb / 204Pb can be a sensitive indicator of the age of lead ores. Such techniques have been used to show that meteorites, believed to be left over from the formation of the solar system, are 4.55 billion years old.
- 53. 53 Radioactive Carbon Dating Radioactive 14C is produced in our atmosphere by the bombardment of 14N by neutrons produced by cosmic rays. When living organisms die, their intake of 14C ceases, and the ratio of 14C / 12C (= R) decreases as 14C decays. The period just before 9000 years ago had a higher 14C / 12C ratio by factor of about 1.5 than it does today. Because the half-life of 14C is 5730 years, it is convenient to use the 14C / 12C ratio to determine the age of objects over a range up to 45,000 years ago.