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E. Nuclear and quantum physics

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  1. E.1 Structure of the atom

    1. • Geiger-Marsden-Rutherford experiment and the discovery of the nucleus.

    2. • Use nuclear notation: A = nucleon number, Z = proton number, X = element symbol.

    3. • Emission and absorption spectra provide evidence for discrete atomic energy levels.

    4. • Photons are emitted/absorbed during transitions between atomic energy levels.

    5. • Photon energy in atomic transition: E=hf.

    6. • Use emission and absorption spectra to infer chemical composition.

  2. E.3 Radioactive decay

    1. • Isotopes.

    2. • Nuclear binding energy and mass defect. • Mass defect connects nuclear mass loss with binding energy.

    3. • Use binding energy per nucleon variation with nucleon number.

    4. • Mass-energy equivalence in nuclear reactions: E=mc^2.

    5. • Strong nuclear force is short-range and attractive between nucleons.

    6. • Radioactive decay is random and spontaneous.

    7. • Alpha, beta and gamma decays change nuclear state differently.

    8. • Write radioactive decay equations for α, β-, β+ and γ.

    9. • Existence of neutrinos ν and antineutrinos ν. • Neutrinos and antineutrinos are required in beta decay.

    10. • Compare penetration and ionizing ability of α, β and γ radiation.

    11. • Activity, count rate and half-life in radioactive decay.

    12. • Use integer half-lives to track activity and count rate changes.

    13. • Effect of background radiation on count rate. • Correct count rate for background radiation.

  3. E.4 Fission

    1. • Energy is released in spontaneous and neutron-induced fission.

    2. • Chain reactions sustain nuclear fission.

    3. • Know control rods, moderators, heat exchangers and shielding in nuclear power plants. • Control rods, moderators, heat exchangers and shielding each have distinct roles.

    4. • Know fission products and nuclear waste management issues. • Include properties and management of fission products.

  4. E.5 Fusion and stars

    1. E.5.1—Stellar equilibrium

      • Stars are stable when outward radiation pressure balances inward gravity.

    2. E.5.2—Fusion in stars

      • Fusion is a source of energy in stars.

    3. E.5.3—Fusion conditions

      • Fusion in stars requires high density and temperature.

    4. E.5.4—Stellar mass and evolution

      • Stellar mass determines star evolution pathway.

    5. E.5.5—HR diagram regions

      • Use HR diagram regions to describe star properties. • Include main sequence, red giants/supergiants, white dwarfs and lines of constant radius.

    6. E.5.6—Stellar parallax

      • Stellar parallax distance: d(pc)=1/p(arcsec).

    7. E.5.7—Stellar radii

      • Determine stellar radius from luminosity and surface temperature.