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11–12Physics 11–12 Syllabus (2025)

Record of changes
Implementation from 2027
Expand for detailed implementation advice
OverviewRationaleAimOutcomesContentAssessmentGlossaryTeaching and learning support

Content

Year 12

Matter, energy and the cosmos

Relevant Working scientifically outcomes and content must be integrated with each focus area. All the Working scientifically outcomes and content must be addressed by the end of Year 12.

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Modelling the atom

  • Account for the origin of cathode rays in a cathode-ray tube

  • Describe the observations made inside a low-pressure tube when a cathode ray interacts with a Maltese cross, a paddle wheel, electric fields, and magnetic fields

  • Analyse how observations of cathode rays provide evidence that cathode rays consist of particles with mass and charge

  • Explain how the charge-to-mass ratio of the electron was first determined

  • Derive the charge-to-mass ratio qm=ErB2 for an electron in a cathode ray tube with perpendicular electric and magnetic fields

  • Evaluate the evidence supporting the plum pudding model of the atom

  • Explain how the observations of the gold foil experiment led to the proposal of a nuclear model of the atom

  • Explain how limitations of the nuclear model led to the development of the stationary energy level model of the atom

  • Explain how the stationary energy level model of the atom uses a mixture of classical physics and quantum physics to address the limitations of the nuclear model of the atom

  • Explain why the difference between the predicted mass and measured mass of a nucleus was a limitation of early models of the atom, and led to the prediction of neutrons

  • Analyse how the law of the conservation of energy and the law of the conservation of momentum were applied in experiments to determine the existence and properties of the neutron

  • Explain why unique line emission spectra and absorption spectra are produced by an element

  • Identify the limitations of the stationary energy level model of the atom

  • Interpret energy level diagrams showing the transition of electrons between energy levels involving both absorption and emission of energy

  • Explain how the law of conservation of energy applies to electrons transitioning between energy levels

  • Solve problems involving the transition of electrons using E=hf, c=fλ and 1λ=R1nf2-1ni2

  • Explain how standing waves can be used to represent electrons in stationary energy levels using qualitative data

  • Use λ=hmv to relate wave and particle properties of matter

  • Explain why the production of electron diffraction patterns provides evidence for electrons behaving as waves

  • Explain how the proposal of electrons as waves in atoms addresses a limitation of the stationary energy level model

  • Describe baryons in terms of quark combinations and the role of the strong force

  • Describe atomic structure in terms of quarks and leptons

  • Explain how particle accelerators and collision experiments are used to discover and study quarks, leptons and force-carrying bosons

  • Analyse how experimental evidence can lead to refinements in scientific models

Radioactivity

  • Relate the isotopic mass number of an element to its subatomic components

  • Describe the range and effect of the strong nuclear force on nucleons

  • Explain how the balance between the strong nuclear force and the electrostatic repulsion force impacts the stability of the nucleus

  • Describe the process of alpha decay, beta decay and gamma decay

  • Compare the composition, charge, mass, ionising ability, and penetration of alpha radiation, beta radiation and gamma radiation

  • Use nuclear decay equations to describe reactions, including radioactive decay and transmutation

  • Apply conservation of mass, energy and charge to nuclear reactions, transmutation and radioactive decay

  • Describe the role of the weak force in beta-minus decay and beta-plus transformation

  • Describe the concept of half-life as it relates to a radioisotope

  • Interpret graphs of radioactive decay to determine the changing amounts of radioisotopes over time

  • Relate the decay constant λ to the half-life of radioisotopes
  • Solve problems involving radioactive decay using λ=ln⁡2T1/2

  • Conduct a practical investigation to model the process of the radioactive decay of an isotope and analyse its half-life

  • Outline the contribution of selected scientists to radio-medicine

  • Explain how the properties of radioisotopes determine their suitability for use in medical scans and industry

Nuclear energy
  • Identify that the special theory of relativity demonstrates the mass–energy equivalence relationship E=mc2

  • Account for the law of conservation of mass and the law of conservation of energy being replaced by the law of conservation of mass–energy

  • Explain the relationship between mass defect and the energy released in a nuclear reaction using E=mc2

  • Explain the process of nuclear fission

  • Compare the processes of controlled chain reactions and uncontrolled chain reactions

  • Explain the structure and function of the components of a fission reactor, including fuel, control rods, moderator and coolant

  • Explain the process of nuclear fusion

  • Outline the contribution of selected scientists to the discovery of nuclear fission

  • Use nuclear equations to describe fusion of small nuclei and fission of large nuclei

  • Explain why fusion requires high temperatures and pressures

  • Compare the energy release of nuclear reactions with the energy release of fossil fuels and conventional explosives

  • Explain nuclear binding energy

  • Solve problems involving mass defect and nuclear binding energy using Δm=mi-mf and E=mc2

  • Distinguish between the proton-neutron ratio and binding energy in the context of nuclear stability

  • Analyse graphical representations of nuclear binding energy per nucleon as atomic number increases, and apply this to the iron limit

  • Account for net release of energy in fission reactions and fusion reactions

  • Describe the properties of a positron

  • Discuss the process of positron–electron annihilation

  • Explain how the law of conservation of mass–energy applies to particle–antiparticle annihilation

  • Explain how positron emission tomography (PET) uses positron–electron annihilation to produce a medical scan

  • Solve problems using mass defect and E=mc2 for nuclear decay, nuclear fission, nuclear fusion, and positron–electron annihilation
Astrophysics

  • Analyse how the spectra of astronomical objects can be used to draw conclusions about their translational velocity, chemical composition and surface temperature

  • Describe Payne Gaposchkin's spectral analysis technique for determining the chemical composition of stars

  • Explain how measured spectra of galaxies provides evidence that the universe is expanding

  • Analyse H-R diagrams to classify stars and determine their surface temperature, colour, luminosity and size

  • Explain the role of gravity and nuclear fusion in the formation of a main sequence star

  • Explain how the mass of a main sequence star determines its position on an H-R diagram and the amount of time that it remains on the main sequence

  • Analyse the nucleosynthesis reactions that occur in main sequence stars by interpreting representations of the proton–proton chain and the carbon–nitrogen–oxygen (CNO) cycle

  • Relate Aboriginal Peoples’ Knowledge of different star colours to the type of nucleosynthesis reactions occurring in main sequence stars

  • Describe, using a H-R diagram, the evolutionary path of a star of one solar mass and a star of greater than 3 solar masses, once they have completed hydrogen fusion

  • Explain how changing forces of gravity and the outwards pressure created by nuclear fusion allows for the synthesis of successively heavier elements

  • Explain, in terms of binding energy, why iron is the heaviest element that can be synthesised in a red supergiant

  • Explain how elements up to, and including iron, are synthesised by stars, and how atoms larger than iron are synthesised

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