EdvanaStart free

Group 4

IB Physics SL Practice Papers

Custom papers focused on specific topics. Pick the outcomes you want to drill, set the marks, and generate exactly what you need.

Official source: IB Physics curriculum

How it works

  1. 1

    Select topics and syllabus outcomes

  2. 2

    Generate a focused practice paper

  3. 3

    Review marks and close the gaps

Start practicing Physics SL

Sign up to generate practice papers, get AI marking, and track your progress through the syllabus.

Start free

More Physics SL tools

Past Papers

Practice under real conditions

Full-length papers matching IB format, timing, and mark allocation — scoped to the current syllabus with criterion-referenced feedback.

Syllabus

See where you stand

Every syllabus outcome mapped visually. Track which topics are solid, which need work, and how ready you are for mocks.

Syllabus viewer

Topic and outcome data shown here comes from Edvana's local syllabus data for this subject, filtered by listed level.

Physics SL

19 topics163 outcomesLocal syllabus version: 2025

A.1 Kinematics

9 outcomes

Open
  1. A.1.U1The motion of bodies through space and time can be described and analysed in terms of position, velocity, and acceleration.
  2. A.1.U2Velocity is the rate of change of position, and acceleration is the rate of change of velocity.
  3. A.1.U3The change in position is the displacement.
  4. A.1.U4The difference between distance and displacement.
  5. A.1.U5The difference between instantaneous and average values of velocity, speed and acceleration, and how to determine them.
  6. A.1.U6The equations of motion for solving problems with uniformly accelerated motion: s=(u+v)/2·t, v=u+at, s=ut+½at², v²=u²+2as.
  7. A.1.U7Motion with uniform and non-uniform acceleration.
  8. A.1.U8The behaviour of projectiles in the absence of fluid resistance, and the application of the equations of motion resolved into vertical and horizontal components.
  9. A.1.U9The qualitative effect of fluid resistance on projectiles, including time of flight, trajectory, velocity, acceleration, range and terminal speed.

A.2 Forces and momentum

14 outcomes

Open
  1. A.2.U1Newton's three laws of motion.
  2. A.2.U2Forces as interactions between bodies.
  3. A.2.U3Forces acting on a body can be represented in a free-body diagram.
  4. A.2.U4Free-body diagrams can be analysed to find the resultant force on a system.
  5. A.2.U5The nature and use of contact forces: normal force F_N, surface frictional force F_f (F_f ≤ μ_s·F_N or F_f = μ_d·F_N), tension, elastic restoring force F_H = −kx (Hooke's law), viscous drag F_d = 6πηrv (Stokes), buoyancy F_b = ρVg.
  6. A.2.U6The nature and use of field forces: gravitational force F_g = mg, electric force F_e, magnetic force F_m.
  7. A.2.U7Linear momentum p = mv remains constant unless the system is acted upon by a resultant external force.
  8. A.2.U8A resultant external force constitutes an impulse J = FΔt; the applied impulse equals the change in momentum.
  9. A.2.U9Newton's second law: F = ma (constant mass) and F = Δp/Δt (variable mass).
  10. A.2.U10Elastic and inelastic collisions of two bodies, and explosions; energy considerations in each.
  11. A.2.U11Bodies moving along a circular trajectory at constant speed experience a centripetal acceleration a = v²/r = ω²r = 4π²r/T².
  12. A.2.U12Circular motion is caused by a centripetal force acting perpendicular to the velocity.
  13. A.2.U13A centripetal force causes the body to change direction even if its magnitude of velocity may remain constant.
  14. A.2.U14Motion along a circular trajectory described using angular velocity ω, related to linear speed by v = 2πr/T = ωr.

A.3 Work, energy and power

11 outcomes

Open
  1. A.3.U1The principle of the conservation of energy.
  2. A.3.U2Work done by a force is equivalent to a transfer of energy.
  3. A.3.U3Energy transfers can be represented on a Sankey diagram.
  4. A.3.U4Work W done on a body by a constant force: W = Fs cos θ.
  5. A.3.U5Work done by the resultant force on a system equals the change in the energy of the system.
  6. A.3.U6Mechanical energy is the sum of kinetic energy, gravitational potential energy and elastic potential energy.
  7. A.3.U7In the absence of frictional/resistive forces, the total mechanical energy of a system is conserved.
  8. A.3.U8If mechanical energy is conserved: E_k = ½mv² = p²/2m; ΔE_p = mgΔh; E_H = ½k(Δx)².
  9. A.3.U9Power P = ΔW/Δt = Fv.
  10. A.3.U10Efficiency η = E_output/E_input = P_output/P_input.
  11. A.3.U11Energy density of fuel sources.

B.1 Thermal energy transfers

15 outcomes

Open
  1. B.1.U1Molecular theory in solids, liquids and gases.
  2. B.1.U2Density ρ = m/V.
  3. B.1.U3Kelvin and Celsius scales are used to express temperature; a change in temperature is the same on both scales.
  4. B.1.U4Kelvin temperature is a measure of the average kinetic energy of particles: Ē_k = (3/2)k_B T.
  5. B.1.U5Internal energy is the total intermolecular potential energy plus the total random kinetic energy of the molecules.
  6. B.1.U6Temperature difference determines the direction of the resultant thermal energy transfer between bodies.
  7. B.1.U7A phase change represents a change in particle behaviour arising from a change in energy at constant temperature.
  8. B.1.U8Quantitative analysis of thermal energy transfers using specific heat capacity c and specific latent heat L: Q = mcΔT and Q = mL.
  9. B.1.U9Conduction, convection and thermal radiation are the primary mechanisms for thermal energy transfer.
  10. B.1.U10Conduction in terms of the difference in kinetic energy of particles.
  11. B.1.U11Quantitative analysis of rate of thermal energy transfer by conduction: ΔQ/Δt = kA·ΔT/Δx.
  12. B.1.U12Qualitative description of thermal energy transferred by convection due to fluid density differences.
  13. B.1.U13Energy transferred by radiation modelled by the Stefan-Boltzmann law: L = σAT⁴.
  14. B.1.U14The concept of apparent brightness b; luminosity L of a body: b = L / (4πd²).
  15. B.1.U15Emission spectrum of a black body; Wien's displacement law: λ_max · T = 2.9 × 10⁻³ mK.

B.2 Greenhouse effect

9 outcomes

Open
  1. B.2.U1The conservation of energy.
  2. B.2.U2Emissivity as the ratio of the power radiated per unit area by a surface compared to that of an ideal black surface at the same temperature: emissivity = (power radiated per unit area) / (σT⁴).
  3. B.2.U3Albedo as a measure of the average energy reflected off a macroscopic system: albedo = total scattered power / total incident power.
  4. B.2.U4Earth's albedo varies daily and is dependent on cloud formations and latitude.
  5. B.2.U5The solar constant S; the incoming radiative power is dependent on the projected surface, resulting in a mean incoming intensity of S/4.
  6. B.2.U6CH₄, H₂O, CO₂ and N₂O are the main greenhouse gases, each with natural and human-activity origins.
  7. B.2.U7Absorption of infrared radiation by the main greenhouse gases in terms of molecular energy levels and subsequent emission of radiation in all directions.
  8. B.2.U8The greenhouse effect can be explained in terms of both a resonance model and molecular energy levels.
  9. B.2.U9The augmentation of the greenhouse effect due to human activities is known as the enhanced greenhouse effect.

B.3 Gas laws

8 outcomes

Open
  1. B.3.U1Pressure P = F/A where F is the force exerted perpendicular to the surface.
  2. B.3.U2Amount of substance n = N/N_A where N is the number of molecules and N_A is the Avogadro constant.
  3. B.3.U3Ideal gases described by kinetic theory; a modelled system to approximate real gases.
  4. B.3.U4The ideal gas law derived from empirical gas laws: PV/T = constant.
  5. B.3.U5Equations governing ideal gases: PV = Nk_B T and PV = nRT.
  6. B.3.U6Change in momentum from collisions gives rise to pressure; P = (1/3)ρv².
  7. B.3.U7Internal energy U of an ideal monatomic gas: U = (3/2)Nk_B T or U = (3/2)nRT.
  8. B.3.U8Temperature, pressure and density conditions under which an ideal gas is a good approximation of a real gas.

B.5 Current and circuits

14 outcomes

Open
  1. B.5.U1Cells provide a source of emf.
  2. B.5.U2Chemical cells and solar cells as energy sources in circuits.
  3. B.5.U3Circuit diagrams represent the arrangement of components in a circuit.
  4. B.5.U4Direct current I as a flow of charge carriers: I = Δq/Δt.
  5. B.5.U5Electric potential difference V is work done per unit charge: V = W/q.
  6. B.5.U6Properties of electrical conductors and insulators in terms of mobility of charge carriers.
  7. B.5.U7Electric resistance and its origin; R = V/I.
  8. B.5.U8Resistivity: ρ = RA/L.
  9. B.5.U9Ohm's law.
  10. B.5.U10Ohmic and non-ohmic behaviour, including the heating effect of resistors.
  11. B.5.U11Electrical power dissipated: P = IV = I²R = V²/R.
  12. B.5.U12Combinations of resistors in series and parallel circuits (series: R_s = R_1 + R_2 + ...; parallel: 1/R_p = 1/R_1 + 1/R_2 + ...).
  13. B.5.U13Electric cells characterised by emf ε and internal resistance r: ε = I(R + r).
  14. B.5.U14Resistors can have variable resistance (thermistors, LDRs, potentiometers).

C.1 Simple harmonic motion

7 outcomes

Open
  1. C.1.U1Conditions that lead to simple harmonic motion.
  2. C.1.U2The defining equation of SHM: a = −ω²x.
  3. C.1.U3A particle undergoing SHM described using time period T, frequency f, angular frequency ω, amplitude, equilibrium position, and displacement.
  4. C.1.U4Time period: T = 1/f = 2π/ω.
  5. C.1.U5Time period of a mass–spring system: T = 2π√(m/k).
  6. C.1.U6Time period of a simple pendulum: T = 2π√(l/g).
  7. C.1.U7A qualitative approach to energy changes during one cycle of an oscillation.

C.2 Wave model

5 outcomes

Open
  1. C.2.U1Transverse and longitudinal travelling waves.
  2. C.2.U2Wavelength λ, frequency f, time period T, and wave speed v: v = fλ = λ/T.
  3. C.2.U3The nature of sound waves.
  4. C.2.U4The nature of electromagnetic waves.
  5. C.2.U5The differences between mechanical waves and electromagnetic waves.

C.3 Wave phenomena

10 outcomes

Open
  1. C.3.U1Waves travelling in two and three dimensions described through wavefronts and rays.
  2. C.3.U2Wave behaviour at boundaries: reflection, refraction and transmission.
  3. C.3.U3Wave diffraction around a body and through an aperture.
  4. C.3.U4Wavefront-ray diagrams showing refraction and diffraction.
  5. C.3.U5Snell's law, critical angle and total internal reflection; n₁/n₂ = sin θ₂/sin θ₁ = v₂/v₁.
  6. C.3.U6Superposition of waves and wave pulses.
  7. C.3.U7Double-source interference requires coherent sources.
  8. C.3.U8Condition for constructive interference: path difference = nλ.
  9. C.3.U9Condition for destructive interference: path difference = (n + ½)λ.
  10. C.3.U10Young's double-slit interference: s = λD/d where s is fringe separation, d is slit separation, D is slit-to-screen distance.

C.4 Standing waves and resonance

6 outcomes

Open
  1. C.4.U1Nature and formation of standing waves as superposition of two identical waves travelling in opposite directions.
  2. C.4.U2Nodes and antinodes, relative amplitude and phase difference of points along a standing wave.
  3. C.4.U3Standing wave patterns in strings and pipes.
  4. C.4.U4The nature of resonance including natural frequency and amplitude of oscillation based on driving frequency.
  5. C.4.U5Effect of damping on the maximum amplitude and resonant frequency of oscillation.
  6. C.4.U6Effects of light, critical and heavy damping on the system.

C.5 Doppler effect

4 outcomes

Open
  1. C.5.U1The nature of the Doppler effect for sound waves and electromagnetic waves.
  2. C.5.U2Representation of the Doppler effect using wavefront diagrams when either source or observer is moving.
  3. C.5.U3Relative change in frequency or wavelength for a light wave (v << c): Δf/f = Δλ/λ ≈ v/c.
  4. C.5.U4Shifts in spectral lines provide information about the motion of stars and galaxies.

D.1 Gravitational fields

5 outcomes

Open
  1. D.1.U1Kepler's three laws of orbital motion.
  2. D.1.U2Newton's universal law of gravitation: F = G(m₁m₂)/r² for bodies treated as point masses.
  3. D.1.U3Conditions under which extended bodies can be treated as point masses.
  4. D.1.U4Gravitational field strength g at a point: g = F/m = GM/r².
  5. D.1.U5Gravitational field lines.

D.2 Electric and magnetic fields

10 outcomes

Open
  1. D.2.U1Direction of forces between the two types of electric charge.
  2. D.2.U2Coulomb's law: F = kq₁q₂/r² where k = 1/(4πε₀).
  3. D.2.U3The conservation of electric charge.
  4. D.2.U4Millikan's experiment as evidence for quantization of electric charge.
  5. D.2.U5Electric charge can be transferred between bodies using friction, electrostatic induction and contact, including grounding.
  6. D.2.U6Electric field strength: E = F/q.
  7. D.2.U7Electric field lines.
  8. D.2.U8Relationship between field line density and field strength.
  9. D.2.U9Uniform electric field strength between parallel plates: E = V/d.
  10. D.2.U10Magnetic field lines.

D.3 Motion in electromagnetic fields

6 outcomes

Open
  1. D.3.U1Motion of a charged particle in a uniform electric field.
  2. D.3.U2Motion of a charged particle in a uniform magnetic field.
  3. D.3.U3Motion of a charged particle in perpendicularly orientated uniform electric and magnetic fields.
  4. D.3.U4Magnitude and direction of the force on a charge moving in a magnetic field: F = qvB sin θ.
  5. D.3.U5Magnitude and direction of the force on a current-carrying conductor in a magnetic field: F = BIL sin θ.
  6. D.3.U6Force per unit length between parallel wires: F/L = μ₀I₁I₂/(2πr).

E.1 Structure of the atom

6 outcomes

Open
  1. E.1.U1The Geiger–Marsden–Rutherford experiment and the discovery of the nucleus.
  2. E.1.U2Nuclear notation: ᴬ_Z X where A is the nucleon number, Z is the proton number and X is the chemical symbol.
  3. E.1.U3Emission and absorption spectra provide evidence for discrete atomic energy levels.
  4. E.1.U4Photons are emitted and absorbed during atomic transitions.
  5. E.1.U5The frequency of the photon released during an atomic transition depends on the energy level difference: E = hf.
  6. E.1.U6Emission and absorption spectra provide information on the chemical composition.

E.3 Radioactive decay

13 outcomes

Open
  1. E.3.U1Isotopes.
  2. E.3.U2Nuclear binding energy and mass defect.
  3. E.3.U3The variation of binding energy per nucleon with nucleon number.
  4. E.3.U4Mass-energy equivalence in nuclear reactions: E = mc².
  5. E.3.U5The existence of the strong nuclear force: short-range, attractive force between nucleons.
  6. E.3.U6The random and spontaneous nature of radioactive decay.
  7. E.3.U7Changes in the state of the nucleus following α, β⁻, β⁺, γ radioactive decay.
  8. E.3.U8Radioactive decay equations for α, β⁻, β⁺, γ.
  9. E.3.U9The existence of neutrinos ν and antineutrinos ν̄.
  10. E.3.U10Penetration and ionizing ability of alpha particles, beta particles and gamma rays.
  11. E.3.U11Activity, count rate and half-life in radioactive decay.
  12. E.3.U12Changes in activity and count rate using integer values of half-life.
  13. E.3.U13The effect of background radiation on count rate.

E.4 Fission

4 outcomes

Open
  1. E.4.U1Energy is released in spontaneous and neutron-induced fission.
  2. E.4.U2The role of chain reactions in nuclear fission reactions.
  3. E.4.U3The role of control rods, moderators, heat exchangers and shielding in a nuclear power plant.
  4. E.4.U4The properties of the products of nuclear fission and their management.

E.5 Fusion and stars

7 outcomes

Open
  1. E.5.U1The stability of stars relies on an equilibrium between outward radiation pressure and inward gravitational forces.
  2. E.5.U2Fusion is a source of energy in stars.
  3. E.5.U3The conditions leading to fusion in stars in terms of density and temperature.
  4. E.5.U4The effect of stellar mass on the evolution of a star.
  5. E.5.U5The main regions of the Hertzsprung–Russell (HR) diagram and the main properties of stars in these regions.
  6. E.5.U6Stellar parallax as a method to determine distance: d(parsec) = 1/p(arc-second).
  7. E.5.U7How to determine stellar radii.