IB Physics SL

Build accurate physical models, select and check equations, interpret experimental evidence and prepare deliberately for each current IB Physics SL assessment demand across the five connected themes.

Course resources

Related tools

Where to start

Start from one known Topic or use a mixed question set to expose the first repeatable Physics error pattern.

Choose your starting point

  1. I know the Topic

    Open its exact syllabus position, identify the required model and review only the relationships within SL scope.

    Browse the syllabus

  2. I do not know what is weak

    Attempt a short mixed set and begin with the first repeated conceptual, mathematical or data-handling error.

    Open Physics Diagnostic

Model, retrieve, apply and repair

  1. Build the model

    Draw the system, define the variables and explain the governing physical principle before selecting an equation.

    Review the model objective

  2. Retrieve and check

    Reconstruct relationships from the data booklet, then check rearrangement, dimensions, units, sign and direction.

    Review relationships in the syllabus

  3. Apply, classify and retry

    Answer a matched question, classify the lost mark precisely and repeat after repairing that failure category.

    Practise questions

How to revise IB Physics SL

Build reliable physical models, interpret experimental evidence and practise selecting equations for current IB Physics SL questions without importing unnecessary HL content.

Practise each Physics demand differently

Choose the representation and checking routine that match the physical reasoning required by each Topic and paper component.

  • Motion, forces and energy

    Kinematics, momentum, work, power and gravitational motion

    Sketch the situation and choose a system before writing equations. Track vector direction and energy transfers, then test the sign, unit and limiting behaviour of every numerical answer.

    Practise mechanics

  • Thermal physics and circuits

    Energy transfer, greenhouse effect, gas laws and electric circuits

    Translate between the particle or charge model, the measurable variables and the equation. Change one condition at a time and explain the resulting direction of change before calculating.

    Practise matter and circuits

  • Waves and fields

    Oscillations, interference, standing waves, Doppler effect and field motion

    Draw the wave, force or field representation first. Mark phase, direction and boundary conditions, then connect the diagram to the chosen relationship and explain the physical meaning clearly.

    Practise waves and fields

  • Paper 1B data analysis and investigation skills

    Graphs, gradients, uncertainty, method design and evidence evaluation

    Identify axes, units and uncertainties before describing a pattern. Calculate gradients or intercepts with visible working, compare evidence quantitatively, and make each proposed improvement address one named limitation directly.

    Practise data questions

Build a consistent study approach

IB Physics SL becomes easier when each Topic is treated as a model rather than a formula list. Use the syllabus map to name the system, draw the relevant objects or fields, state assumptions and predict the direction or scale of the result before calculating. Then select a data-booklet relationship, show the rearrangement, keep units visible and interpret whether the answer is physically reasonable. This keeps revision inside the SL scope while building the reasoning required across the five themes.

Use syllabus objectives to rebuild the model, the syllabus checklist to retrieve definitions and relationships, and the Question Bank to apply them to multiple-choice, data-based and structured questions. After marking, label each loss as model selection, algebra, units, graph interpretation, uncertainty or explanation. Repair that category and retry one matched question before moving to a mixed set.

IB Physics SL assessment format

External assessment contributes 80% and the scientific investigation contributes 20%. Prepare separately for conceptual discrimination, data analysis and structured physical reasoning at SL.

Paper / componentQuestionsTime% of grade
Paper 145 marksPaper 1A contains 25 multiple-choice marks and Paper 1B contains 20 data-based marks.How to prepare: Practise 1A by comparing models and eliminating physically inconsistent options; practise 1B through gradients, uncertainty, experimental evidence and concise conclusions.1 hour 30 minutes36%
Paper 250 marksStructured and extended-response questions covering the SL syllabus.How to prepare: Show the model, equation choice, rearrangement, units and physical interpretation clearly in each structured response.1 hour 30 minutes44%
Scientific investigation24 marksOne individual open-ended scientific investigation, internally assessed and externally moderated.How to prepare: Develop a focused question, controlled method, defensible uncertainty treatment, evidence-based conclusion and evaluation linked to specific limitations.10 recommended course hours20%

SourceInternational Baccalaureate Organization · IB Physics subject brief — first assessment 2025IB Physics · First assessment 2025

Grade boundaries

Reproduced report ↗
IB / Physics / SLBrowse other courses ↗

Third-party report · Brilliant Learning. Reported maxima are range endpoints; IB issuer authentication, nominal exam maxima and timezone geography remain unverified.

REPORTED OVERALL BOUNDARY

67 · reported upper bound 100Reported marks

Swipe the table to compare all grades →

2026 · May · Report timezone 1 · Paper breakdown. Reported grade thresholds and range upper bounds; nominal maxima and weights unverified
AssessmentReported upper boundWeightGrade 7Grade 6Grade 5Grade 4Grade 3Grade 2Grade 1
OverallReported marks ↗100—67–10057–6646–5636–4522–3513–210–12
PAPER 1 (MCQ)Reported marks ↗25—13–2512–1210–119–98–87–70–6
PAPER 1 BReported marks ↗20—18–2016–1713–1511–128–104–70–3
Paper 2Reported marks ↗50—32–5026–3121–2515–207–144–60–3
PRACTICAL WORKReported marks ↗24—20–2417–1914–1611–137–104–60–3
About these marks

— = not applicable or weight not verified. Component marks use their own scale; the overall result may be weighted. Swipe to see all grades →

i

16 coverage gaps are recorded for this course. Missing or unverified marks are not estimated.

Coverage for 2026 · May

Missing or unverified marks are not estimated. Historical data do not establish current syllabus equivalence.

Official report authentication pending
2026 · Mayissuer annual source not authenticated
Historical assessment version pending
2022, 2023, 2024, 2025, 2026historical syllabus binding unverified
Route and timezone mapping pending
2022, 2023, 2024, 2025, 2026special route and timezone meaning unverified
Full component inventory pending
2022, 2023, 2024, 2025, 2026full official paper coverage unconfirmed

Frequently Asked Questions

Choose one syllabus Topic if the weakness is known; otherwise attempt a short mixed set. Rebuild the physical model, retrieve the relevant relationship, answer a matched question and classify the first lost mark before deciding what to review next.

Learn where relationships and constants are located, but focus on choosing and using them. During practice, name the model first, select the relationship, rearrange visibly, check dimensions and units, then interpret whether the numerical result is physically reasonable. The official specimen instructions for Paper 1A, Paper 1B and Paper 2 require a calculator and a clean copy of the Physics data booklet. Use the version your teacher confirms for your examination session; the Exam page link below opens the official specimen papers and markschemes for first examinations in 2025.

Identify variables, units and uncertainties before describing the evidence. Practise gradients, intercepts and proportional relationships with visible working, then separate the measured pattern from its physical explanation and tie each evaluation point to a specific limitation.

Move to mixed sections after you can set up unfamiliar questions from several Topics without notes. Use full timed papers later, once errors are mostly pace or decision-making problems rather than repeated gaps in models, algebra, units or data handling.

Investigate your own focused research question using quantitative data, then explain the analysis, conclusion and limitations in a report of no more than 3,000 words. A short, well-supported investigation is more useful than filling the word limit. Plan a question for which you can obtain suitable evidence, and check your school’s submission instructions with your teacher.

Explore the IB Physics SL syllabus

The current IB Physics SL syllabus uses five themes explored through forces, energy and particles. Use the Unit and Topic map to connect motion, matter, waves, fields, nuclear physics and practical skills while keeping revision inside the assessed SL scope.

  1. A. Space, time and motion

    3 topics · 49 objectivesSL / HL shared

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    1. A.1 KinematicsSL / HL shared

      1. A.1.1—Position, velocity and acceleration SL / HL shared

        • Describe motion using position, velocity and acceleration.

      2. A.1.2—Velocity and acceleration rates SL / HL shared

        • Velocity is the rate of change of position, and acceleration is the rate of change of velocity.

      3. A.1.3—Displacement SL / HL shared

        • Change in position is the displacement.

      4. A.1.4—Distance and displacement SL / HL shared

        • Distinguish distance and displacement.

      5. A.1.5—Instantaneous and average values SL / HL shared

        • Distinguish instantaneous vs average speed, velocity and acceleration.

      6. A.1.6—Uniform acceleration equations SL / HL shared

        • Use SUVAT equations for uniform acceleration: s=(u+v)t/2; v=u+at; s=ut+1/2at^2; v^2=u^2+2as. • Apply only to uniformly accelerated motion.

      7. A.1.7—Uniform vs non-uniform acceleration SL / HL shared

        • Motion with uniform and non-uniform acceleration.

      8. A.1.8—Projectile components SL / HL shared

        • Resolve projectile motion into horizontal and vertical components when fluid resistance is absent.

      9. A.1.9—Fluid resistance on projectiles SL / HL shared

        • Describe effects on trajectory, flight time, velocity, acceleration, range and terminal speed.

    2. A.2 Forces and momentumSL / HL shared

      1. A.2.1—Newton’s three laws of motion SL / HL shared

        • Newton’s three laws of motion.

      2. A.2.2—Forces as interactions between bodies SL / HL shared

        • Forces as interactions between bodies.

      3. A.2.3—Free-body diagrams SL / HL shared

        • Forces acting on a body can be represented in a free-body diagram.

      4. A.2.4—Resultant force from diagrams SL / HL shared

        • Free-body diagrams can be analysed to find the resultant force on a system.

      5. A.2.5—Contact forces SL / HL shared

        • Contact forces include normal, friction, tension, elastic restoring force, viscous drag and buoyancy.

      6. A.2.6—Normal force SL / HL shared

        • Normal force FN acts perpendicular to the contact surface.

      7. A.2.7—Frictional force SL / HL shared

        • Friction acts parallel to contact. • Static: Ff <= μsFN; dynamic: Ff = μdFN.

      8. A.2.8—Tension SL / HL shared

        • Tension.

      9. A.2.9—Hooke’s law restoring force SL / HL shared

        • Elastic restoring force follows Hooke’s law: FH = -kx.

      10. A.2.10—Viscous drag SL / HL shared

        • Viscous drag on a small sphere: Fd = 6πηrv, opposite motion. • η is fluid viscosity, r sphere radius, v speed through fluid.

      11. A.2.11—Buoyancy SL / HL shared

        • Buoyancy from displaced fluid: Fb = ρVg.

      12. A.2.12—Field forces SL / HL shared

        • Know field forces: gravitational, electric and magnetic.

      13. A.2.13—Weight SL / HL shared

        • Weight is gravitational force: Fg = mg.

      14. A.2.14—Electric force Fe SL / HL shared

        • Electric force Fe.

      15. A.2.15—Magnetic force Fm SL / HL shared

        • Magnetic force Fm.

      16. A.2.16—Linear momentum conservation SL / HL shared

        • Linear momentum p=mv is conserved unless a resultant external force acts.

      17. A.2.17—Impulse SL / HL shared

        • Impulse from resultant external force: J = FΔt = Δp.

      18. A.2.18—Impulse-momentum change SL / HL shared

        • The applied external impulse equals the change in momentum of the system.

      19. A.2.19—Newton’s second law forms SL / HL shared

        • Use F=ma for constant mass; use F=Δp/Δt when mass changes.

      20. A.2.20—Elastic and inelastic collisions SL / HL shared

        • Elastic and inelastic collisions of two bodies.

      21. A.2.21—Explosions SL / HL shared

        • Explosions.

      22. A.2.22—Collision energy SL / HL shared

        • Compare energy in elastic collisions, inelastic collisions and explosions.

      23. A.2.23—Centripetal acceleration SL / HL shared

        • Centripetal acceleration is radial: a=v^2/r=ω^2r=4π^2r/T^2. • Direction is radially toward the centre of the circle.

      24. A.2.24—Centripetal force SL / HL shared

        • Circular motion is caused by a centripetal force acting perpendicular to the velocity.

      25. A.2.25—Direction change in circular motion SL / HL shared

        • A centripetal force causes the body to change direction even if its magnitude of velocity may remain constant.

      26. A.2.26—Angular and linear speed SL / HL shared

        • Circular motion relation: v=2πr/T=ωr. • Use angular velocity ω and period T to link angular and linear descriptions.

    3. A.3 Work, energy and powerSL / HL shared

      1. A.3.1—Conservation of energy SL / HL shared

        • Principle of the conservation of energy.

      2. A.3.2—Work as energy transfer SL / HL shared

        • Work done by a force is equivalent to a transfer of energy.

      3. A.3.3—Sankey diagrams SL / HL shared

        • Energy transfers can be represented on a Sankey diagram.

      4. A.3.4—Work by constant force SL / HL shared

        • Work by constant force along displacement: W = Fs cos θ.

      5. A.3.5—Work-energy change SL / HL shared

        • Work done by the resultant force on a system is equal to the change in the energy of the system.

      6. A.3.6—Mechanical energy SL / HL shared

        • Mechanical energy includes kinetic, gravitational potential and elastic potential energy.

      7. A.3.7—Mechanical energy conservation SL / HL shared

        • Mechanical energy is conserved when friction/resistive forces are absent.

      8. A.3.8—Mechanical energy transformations SL / HL shared

        • If mechanical energy is conserved, work transforms energy between mechanical forms. • Relevant forms: translational kinetic, near-Earth gravitational potential and elastic potential.

      9. A.3.9—Kinetic energy SL / HL shared

        • Translational kinetic energy: Ek = 1/2mv^2 = p^2/2m.

      10. A.3.10—Gravitational potential energy SL / HL shared

        • Near Earth, gravitational potential energy change: ΔEp = mgΔh.

      11. A.3.11—Elastic potential energy SL / HL shared

        • Elastic potential energy: EH = 1/2k(Δx)^2.

      12. A.3.12—Power SL / HL shared

        • Power is rate of work or energy transfer: P=ΔW/Δt=Fv.

      13. A.3.13—Efficiency SL / HL shared

        • Efficiency: η=Eoutput/Einput=Poutput/Pinput.

      14. A.3.14—Fuel energy density SL / HL shared

        • Energy density of the fuel sources.

  2. B. The particulate nature of matter

    4 topics · 50 objectivesSL / HL shared

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    1. B.1 Thermal energy transfersSL / HL shared

      1. B.1.1—Molecular states SL / HL shared

        • Describe solids, liquids and gases using molecular theory.

      2. B.1.2—Density SL / HL shared

        • Density: ρ=m/V.

      3. B.1.3—Temperature scales SL / HL shared

        • Use Kelvin and Celsius temperature scales.

      4. B.1.4—Temperature scale changes SL / HL shared

        • Temperature change has the same size in Kelvin and Celsius.

      5. B.1.5—Kelvin temperature and kinetic energy SL / HL shared

        • Kelvin temperature measures average particle kinetic energy: Ek=3/2 kBT.

      6. B.1.6—Internal energy SL / HL shared

        • Internal energy = intermolecular potential energy + random molecular kinetic energy.

      7. B.1.7—Thermal transfer direction SL / HL shared

        • Temperature difference sets the net direction of thermal energy transfer.

      8. B.1.8—Phase change SL / HL shared

        • Phase change changes particle behaviour via energy transfer at constant temperature.

      9. B.1.9—Specific heat and latent heat SL / HL shared

        • Use Q=mcΔT for temperature change and Q=mL for phase change.

      10. B.1.10—Thermal transfer mechanisms SL / HL shared

        • Conduction, convection and thermal radiation are the primary mechanisms for thermal energy transfer.

      11. B.1.11—Conduction SL / HL shared

        • Conduction: the difference in the kinetic energy of particles.

      12. B.1.12—Conduction rate SL / HL shared

        • Conduction rate depends on material, area and temperature gradient: ΔQ/Δt = kAΔT/Δx.

      13. B.1.13—Convection SL / HL shared

        • Qualitative description of thermal energy transferred by convection due to fluid density differences.

      14. B.1.14—Black-body radiation SL / HL shared

        • Black-body radiation power follows Stefan-Boltzmann law: L=σAT^4. • Applies to emission of electromagnetic waves from a black-body surface.

      15. B.1.15—Apparent brightness SL / HL shared

        • Concept of apparent brightness b.

      16. B.1.16—Luminosity and brightness SL / HL shared

        • Apparent brightness relation: b = L/(4πd^2).

      17. B.1.17—Wien’s displacement law SL / HL shared

        • Use black-body spectrum and Wien’s law: λmaxT = 2.9x10^-3 m K. • Use λmax to infer black-body temperature.

    2. B.2 Greenhouse effectSL / HL shared

      1. B.2.1—Conservation of energy SL / HL shared

        • Conservation of energy.

      2. B.2.2—Emissivity SL / HL shared

        • Emissivity compares surface radiation per unit area with a black body: ε = power/(σT^4).

      3. B.2.3—Albedo SL / HL shared

        • Albedo = total scattered power / total incident power.

      4. B.2.4—Earth’s albedo variation SL / HL shared

        • Earth’s albedo varies daily with cloud formation and latitude.

      5. B.2.5—Solar constant S SL / HL shared

        • Solar constant S.

      6. B.2.6—Mean solar intensity SL / HL shared

        • Mean incoming solar intensity is S/4 due to planetary geometry.

      7. B.2.7—Greenhouse gases SL / HL shared

        • Main greenhouse gases: CH4, H2O, CO2 and N2O from natural and human sources. • Greenhouse gases have both natural and human-created origins.

      8. B.2.8—Infrared absorption SL / HL shared

        • Greenhouse gases absorb IR via molecular energy levels. • Radiation is re-emitted in all directions.

      9. B.2.9—Greenhouse models SL / HL shared

        • Explain greenhouse effect using resonance and molecular energy-level models.

      10. B.2.10—Enhanced greenhouse effect SL / HL shared

        • Enhanced greenhouse effect = augmentation due to human activity.

    3. B.3 Gas lawsSL / HL shared

      1. B.3.1—Pressure SL / HL shared

        • Pressure: P=F/A for force perpendicular to a surface.

      2. B.3.2—Amount of substance SL / HL shared

        • Amount of substance: n=N/NA.

      3. B.3.3—Ideal gas model SL / HL shared

        • Ideal gases are kinetic-theory models that approximate real gas behaviour.

      4. B.3.4—Empirical gas laws SL / HL shared

        • Empirical gas laws combine to PV/T = constant.

      5. B.3.5—Ideal gas equations SL / HL shared

        • Ideal gas equations: PV=NkBT and PV=nRT.

      6. B.3.6—Molecular pressure model SL / HL shared

        • Pressure arises from molecular momentum changes in collisions with surfaces. • Average translational speed relation: P = 1/3 ρv^2.

      7. B.3.7—Ideal gas internal energy SL / HL shared

        • Internal energy of ideal monatomic gas: U=3/2 NkBT = 3/2 nRT.

      8. B.3.8—Ideal gas approximation limits SL / HL shared

        • State temperature, pressure and density conditions for ideal-gas approximation.

    4. B.5 Current and circuitsSL / HL shared

      1. B.5.1—Cells provide a source of emf SL / HL shared

        • Cells provide a source of emf.

      2. B.5.2—Electrical energy sources SL / HL shared

        • Chemical cells and solar cells are energy sources in circuits. • Compare the advantages and disadvantages of different sources of electrical energy.

      3. B.5.3—Resistance SL / HL shared

        • Explain the properties of electrical conductors and insulators in terms of the mobility of charge carriers. • Explain electrical resistance and its origin. • Use electrical resistance R=V/I.

      4. B.5.4—Ohmic behaviour SL / HL shared

        • Apply Ohm’s law: for an ohmic metal conductor at constant temperature, V ∝ I. • Distinguish ohmic and non-ohmic behaviour of electrical conductors, including the heating effect of resistors.

      5. B.5.5—Electrical power SL / HL shared

        • Electrical power: P=IV=I^2R=V^2/R.

      6. B.5.6—Potential difference and electrical energy transfer SL / HL shared

        • Electric potential difference V is the work done W per unit charge q on moving a positive charge between two points along the path of the current: V=W/q. • Relate electrical energy transfer to power and time: E=Pt=IVt.

      7. B.5.7—Electric cells SL / HL shared

        • Cells convert chemical energy to electrical energy.

      8. B.5.8—Circuit diagrams and conventional current SL / HL shared

        • Circuit diagrams represent the arrangement of components in a circuit; use the required electrical circuit symbols provided in the Physics data booklet. • Conventional current follows the direction of positive charge flow. • Treat ammeters and voltmeters as ideal unless stated otherwise; a stated non-ideal meter has constant resistance.

      9. B.5.9—Direct current and charge flow SL / HL shared

        • Direct current I is a flow of charge carriers in one direction, with I=Δq/Δt. • Alternating-current circuit analysis is not required.

      10. B.5.10—Direct and alternating current boundary SL / HL shared

        • Distinguish direct current, whose direction does not reverse, from alternating current, whose direction reverses. • This distinction defines the syllabus boundary only; alternating-current circuit analysis is not required.

      11. B.5.11—Conservation in series and parallel circuits SL / HL shared

        • Use conservation of charge to explain why currents add at a junction in a parallel circuit. • Use conservation of energy to explain why potential differences add in a series circuit. • General multi-loop circuit analysis is not required.

      12. B.5.12—Resistance and resistivity SL / HL shared

        • Resistance depends on resistivity and dimensions: R=ρL/A.

      13. B.5.13—Series and parallel circuits SL / HL shared

        • Use series/parallel rules for current, voltage and equivalent resistance. • Series: same current; voltages and resistances add. • Parallel: same voltage; currents add; reciprocal resistance adds.

      14. B.5.14—Emf and internal resistance SL / HL shared

        • Cell emf with internal resistance: ε = I(R+r).

      15. B.5.15—Variable resistance SL / HL shared

        • Resistors can have variable resistance. • Variable resistors are limited to thermistors, light-dependent resistors (LDRs) and potentiometers.

  3. C. Wave behaviour

    5 topics · 33 objectivesSL / HL shared

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    1. C.1 Simple harmonic motionSL / HL shared

      1. C.1.1—Conditions for SHM SL / HL shared

        • Conditions that lead to simple harmonic motion.

      2. C.1.2—SHM defining equation SL / HL shared

        • SHM defining equation: a = -ω^2x.

      3. C.1.3—SHM quantities SL / HL shared

        • Describe SHM using T, f, ω, amplitude, equilibrium position and displacement.

      4. C.1.4—Period, frequency and angular frequency SL / HL shared

        • Oscillation period relations: T=1/f=2π/ω.

      5. C.1.5—Mass–spring period SL / HL shared

        • The time period of a mass–spring system is T=2π√(m/k).

      6. C.1.6—Simple pendulum period SL / HL shared

        • The time period of a simple pendulum in the small-angle approximation is T=2π√(l/g).

      7. C.1.7—Qualitative energy changes in SHM SL / HL shared

        • Describe qualitatively how kinetic and potential energy change during one cycle of an oscillation; total mechanical energy remains constant for an ideal oscillator.

    2. C.2 Wave modelSL / HL shared

      1. C.2.1—Transverse and longitudinal travelling waves SL / HL shared

        • Distinguish transverse and longitudinal travelling waves by comparing particle or field oscillation with the direction of propagation and energy transfer. • Describe the motion of particles in a medium using displacement with position and with time.

      2. C.2.2—Wave quantities and wave equation SL / HL shared

        • Apply wavelength λ, frequency f, time period T and wave speed v to wave motion using v=fλ=λ/T.

      3. C.2.3—Nature of sound waves SL / HL shared

        • Explain sound as a mechanical longitudinal wave, including particle oscillations, compressions and rarefactions, and energy transfer through a medium.

      4. C.2.4—Nature of electromagnetic waves SL / HL shared

        • Explain electromagnetic waves as transverse oscillating electric and magnetic fields that can propagate through a vacuum. • Use the approximate wavelength orders of magnitude in the Physics data booklet without treating them as sharp boundaries.

      5. C.2.5—Mechanical and electromagnetic wave models SL / HL shared

        • Compare mechanical waves, which require a medium, with electromagnetic waves, which can travel through a vacuum. • Travelling waves transfer energy even when there is no resultant displacement of the medium. • Apply the wave model to both mechanical and electromagnetic waves.

    3. C.3 Wave phenomenaSL / HL shared

      1. C.3.1—Wavefronts and rays SL / HL shared

        • Waves travelling in two and three dimensions can be described through the concepts of wavefronts and rays.

      2. C.3.2—Snell’s law SL / HL shared

        • Snell’s law: n1 sinθ1 = n2 sinθ2.

      3. C.3.3—Refractive index SL / HL shared

        • Refractive index: n=c/v.

      4. C.3.4—Total internal reflection SL / HL shared

        • Total internal reflection condition uses critical angle: sinθc=n2/n1.

      5. C.3.5—Superposition SL / HL shared

        • Superposition adds displacements where waves overlap.

      6. C.3.6—Coherence SL / HL shared

        • Coherence requires constant phase difference between waves.

      7. C.3.7—Path difference SL / HL shared

        • Path difference determines constructive or destructive interference.

      8. C.3.8—Two-source interference SL / HL shared

        • Two-source interference depends on path difference and wavelength.

      9. C.3.9—Young double-slit equation SL / HL shared

        • Young double-slit spacing: s = λD/d.

      10. C.3.10—Reflection, refraction and transmission at boundaries SL / HL shared

        • Explain wave behaviour at boundaries in terms of reflection, refraction and transmission. • Sketch and interpret incident, reflected and transmitted wavefronts and rays at normal or oblique incidence within the syllabus guidance.

      11. C.3.11—Diffraction around bodies and through apertures SL / HL shared

        • Explain diffraction around a body and through an aperture. • Use wavefront–ray diagrams to represent diffraction, and relate greater spreading qualitatively to wavelength and aperture size.

    4. C.4 Standing waves and resonanceSL / HL shared

      1. C.4.1—Standing wave formation SL / HL shared

        • Standing waves form by superposition of identical opposite-travelling waves.

      2. C.4.2—Nodes and antinodes SL / HL shared

        • Identify nodes, antinodes, amplitude and phase along standing waves. • Include relative amplitude and phase difference along the standing wave.

      3. C.4.3—Strings and pipes SL / HL shared

        • Know standing-wave patterns in strings and pipes.

      4. C.4.4—Resonance SL / HL shared

        • Resonance relates driving frequency, natural frequency and amplitude.

      5. C.4.5—Damping and resonance SL / HL shared

        • Damping reduces maximum amplitude and shifts resonant frequency.

      6. C.4.6—Types of damping SL / HL shared

        • Compare light, critical and heavy damping effects.

    5. C.5 Doppler effectSL / HL shared

      1. C.5.1—Doppler effect SL / HL shared

        • Nature of the Doppler effect for sound waves and electromagnetic waves.

      2. C.5.2—Doppler wavefront diagrams SL / HL shared

        • Represent Doppler effect with wavefront diagrams for moving source or observer.

      3. C.5.3—Light Doppler approximation SL / HL shared

        • For light at low relative speed: Δf/f = Δλ/λ ≈ v/c.

      4. C.5.4—Spectral line shifts SL / HL shared

        • Spectral line shifts reveal motion of stars and galaxies.

  4. D. Fields

    3 topics · 21 objectivesSL / HL shared

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    1. D.1 Gravitational fieldsSL / HL shared

      1. D.1.1—Kepler’s three laws of orbital motion SL / HL shared

        • Kepler’s three laws of orbital motion.

      2. D.1.2—Universal gravitation SL / HL shared

        • Universal gravitation: F=Gm1m2/r^2 for point masses.

      3. D.1.3—Point-mass approximation SL / HL shared

        • Extended bodies can be treated as point masses only under suitable conditions.

      4. D.1.4—Gravitational field strength SL / HL shared

        • Gravitational field strength: g=F/m=GM/r^2.

      5. D.1.5—Gravitational field lines SL / HL shared

        • Gravitational field lines.

    2. D.2 Electric and magnetic fieldsSL / HL shared

      1. D.2.1—Electric charge forces SL / HL shared

        • Direction of forces between the two types of electric charge.

      2. D.2.2—Coulomb’s law SL / HL shared

        • Coulomb’s law: F=kq1q2/r^2 for point charges; k=1/(4πε0).

      3. D.2.3—Charge conservation SL / HL shared

        • Conservation of electric charge.

      4. D.2.4—Millikan experiment SL / HL shared

        • Millikan’s experiment as evidence for quantization of electric charge.

      5. D.2.5—Charge transfer SL / HL shared

        • Charge transfers by friction, electrostatic induction or contact. • Grounding can remove or add charge.

      6. D.2.6—Electric field strength SL / HL shared

        • Electric field strength: E=F/q.

      7. D.2.7—Electric field lines SL / HL shared

        • Electric field lines.

      8. D.2.8—Field-line density SL / HL shared

        • Relationship between field line density and field strength. • Greater field-line density indicates stronger field.

      9. D.2.9—Parallel-plate field SL / HL shared

        • Uniform field between plates: E=V/d.

      10. D.2.10—Magnetic field lines SL / HL shared

        • Magnetic field lines.

    3. D.3 Motion in electromagnetic fieldsSL / HL shared

      1. D.3.1—Charge in electric fields SL / HL shared

        • Motion of a charged particle in a uniform electric field.

      2. D.3.2—Charge in magnetic fields SL / HL shared

        • Motion of a charged particle in a uniform magnetic field.

      3. D.3.3—Crossed electric and magnetic fields SL / HL shared

        • Charged particles can move in perpendicular uniform electric and magnetic fields.

      4. D.3.4—Magnetic force on charge SL / HL shared

        • Magnetic force on moving charge: F=qvB sinθ.

      5. D.3.5—Force on current conductor SL / HL shared

        • Force on current-carrying conductor: F=BIL sinθ.

      6. D.3.6—Force between parallel wires SL / HL shared

        • Force per unit length between parallel wires: F/L=μ0I1I2/(2πr). • Parallel currents attract when currents flow in the same direction.

  5. E. Nuclear and quantum physics

    4 topics · 30 objectivesSL / HL shared

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    1. E.1 Structure of the atomSL / HL shared

      1. E.1.1—Rutherford experiment SL / HL shared

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

      2. E.1.2—Nuclear notation SL / HL shared

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

      3. E.1.3—Atomic energy levels SL / HL shared

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

      4. E.1.4—Atomic transitions SL / HL shared

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

      5. E.1.5—Photon energy SL / HL shared

        • Photon energy in atomic transition: E=hf.

      6. E.1.6—Spectra and composition SL / HL shared

        • Use emission and absorption spectra to infer chemical composition.

    2. E.3 Radioactive decaySL / HL shared

      1. E.3.1—Isotopes SL / HL shared

        • Isotopes.

      2. E.3.2—Binding energy and mass defect SL / HL shared

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

      3. E.3.3—Binding energy curve SL / HL shared

        • Use binding energy per nucleon variation with nucleon number.

      4. E.3.4—Mass-energy equivalence SL / HL shared

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

      5. E.3.5—Strong nuclear force SL / HL shared

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

      6. E.3.6—Random radioactive decay SL / HL shared

        • Radioactive decay is random and spontaneous.

      7. E.3.7—Decay nuclear changes SL / HL shared

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

      8. E.3.8—Decay equations SL / HL shared

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

      9. E.3.9—Neutrinos and antineutrinos SL / HL shared

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

      10. E.3.10—Radiation penetration and ionization SL / HL shared

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

      11. E.3.11—Activity, count rate and half-life SL / HL shared

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

      12. E.3.12—Half-life changes SL / HL shared

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

      13. E.3.13—Background radiation SL / HL shared

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

    3. E.4 FissionSL / HL shared

      1. E.4.1—Fission energy release SL / HL shared

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

      2. E.4.2—Chain reactions SL / HL shared

        • Chain reactions sustain nuclear fission.

      3. E.4.3—Nuclear power plant roles SL / HL shared

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

      4. E.4.4—Fission products and waste SL / HL shared

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

    4. E.5 Fusion and starsSL / HL shared

      1. E.5.1—Stellar equilibrium SL / HL shared

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

      2. E.5.2—Fusion in stars SL / HL shared

        • Fusion is a source of energy in stars.

      3. E.5.3—Fusion conditions SL / HL shared

        • Fusion in stars requires high density and temperature.

      4. E.5.4—Stellar mass and evolution SL / HL shared

        • Stellar mass determines star evolution pathway.

      5. E.5.5—HR diagram regions SL / HL shared

        • 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 SL / HL shared

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

      7. E.5.7—Stellar radii SL / HL shared

        • Determine stellar radius from luminosity and surface temperature.

  6. S Skills in Physics

    6 topics · 17 objectivesSL / HL shared

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    1. S1.1 Experimental techniquesSL / HL shared

      1. S1.1.1—Safety and ethics SL / HL shared

        • Address safety, ethical and environmental issues.

      2. S1.1.2—Measurement variables SL / HL shared

        • Measure required variables with suitable precision. • Variables include mass, time, length, volume, temperature, force, current, potential difference, angle, sound and light intensity.

    2. S1.2 TechnologySL / HL shared

      1. S1.2.1—Data collection technology SL / HL shared

        • Use sensors, databases, simulations and video/image analysis to collect data.

      2. S1.2.2—Data processing technology SL / HL shared

        • Use spreadsheets, graphs and modelling to process data.

    3. S1.3 MathematicsSL / HL shared

      1. S1.3.1—General mathematics SL / HL shared

        • Use algebra, geometry, trigonometry, logs, rates, estimation and proportional reasoning. • Include equation manipulation and proportional reasoning.

      2. S1.3.2—Vectors and diagrams SL / HL shared

        • Draw, combine, scale and resolve vectors; interpret free-body diagrams.

      3. S1.3.3—Units and numerical values SL / HL shared

        • Use SI units, prefixes, symbols, significant figures and unit checks.

      4. S1.3.4—Uncertainties SL / HL shared

        • Record and propagate absolute, fractional and percentage uncertainties to suitable precision.

      5. S1.3.5—Graphing SL / HL shared

        • Construct, linearize and interpret graphs. • Include uncertainty bars, gradients, intercepts, maxima/minima and areas.

    4. S2.1 Exploring and designingSL / HL shared

      1. S2.1.1—Exploring SL / HL shared

        • Use sources to form research questions, hypotheses and predictions.

      2. S2.1.2—Designing investigations SL / HL shared

        • Design investigations and justify variables, ranges and methods. • Include independent, dependent and controlled variables.

      3. S2.1.3—Controlling variables SL / HL shared

        • Control variables using calibration, insulation, friction/resistance reduction and background corrections.

    5. S2.2 Collecting and processing dataSL / HL shared

      1. S2.2.1—Collecting data SL / HL shared

        • Record sufficient qualitative observations and quantitative data.

      2. S2.2.2—Processing and interpreting data SL / HL shared

        • Process and interpret data, graphs, trends, relationships and outliers.

      3. S2.2.3—Data quality SL / HL shared

        • Assess accuracy, precision, reliability and validity.

    6. S2.3 Concluding and evaluatingSL / HL shared

      1. S2.3.1—Concluding SL / HL shared

        • Justify conclusions and discuss scientific context and uncertainty impacts.

      2. S2.3.2—Evaluating SL / HL shared

        • Evaluate hypotheses, random/systematic errors, limitations and assumptions. • Suggest realistic improvements.