IB Diploma Programme Physics Higher Level
IB Diploma Programme Physics Higher Level (first assessment 2025) is a rigorous 240-hour experimental science course structured around five themes: Space, Time and Motion; The Particulate Nature of Matter; Wave Behaviour; Fields; and Nuclear and Quantum Physics. The HL course extends the SL content with five exclusively HL topics (Rigid Body Mechanics, Special Relativity, Thermodynamics, Electromagnetic Induction, and Quantum Physics) plus deeper mathematical treatment within shared topics, demanding quantitative problem-solving, data analysis, and multi-concept synthesis at a level comparable to first-year university physics.
Who Should Take This
Students who have completed the IB Physics HL course and are preparing for the May/November IB examinations, as well as undergraduate-level learners seeking a rigorous, calculus-adjacent treatment of classical and modern physics aligned to the 2025+ IB syllabus.
What's Covered
1Theme A: Space, Time and Motion
2Theme B: The Particulate Nature of Matter
3Theme C: Wave Behaviour
4Theme D: Fields
5Theme E: Nuclear and Quantum Physics
What's Included in AccelaStudy® AI
Adaptive Knowledge Graph
Practice Questions
Lesson Modules
Console Simulator Labs
Exam Tips & Strategy
13 Activity Formats
Course Outline
1Theme A: Space, Time and Motion 5 topics
A.1 Kinematics
- Recall the definitions of displacement, velocity, and acceleration, distinguishing scalar from vector quantities and applying correct SI units in one-dimensional and two-dimensional motion contexts
- Apply the four SUVAT equations of uniform acceleration to solve multi-step kinematics problems including vertical free-fall and horizontal-launch projectile scenarios
- Analyse projectile motion by independently resolving horizontal constant-velocity and vertical uniform-acceleration components, accounting qualitatively for air resistance effects on range and peak height
A.2 Forces and Momentum
- Recall Newton's three laws of motion and construct free-body diagrams identifying all contact and field forces acting on objects in static equilibrium and accelerating-system scenarios
- Apply conservation of linear momentum and the impulse-momentum theorem to solve elastic and inelastic collision problems in both one and two dimensions, including 2D vector resolution
- Apply centripetal force and angular velocity relationships to analyse uniform circular motion in banked tracks, conical pendulums, and vertical-circle problems where normal force varies with position
A.3 Work, Energy and Power
- Apply work, kinetic-energy theorem, and power formulas to mechanical systems, including efficiency analysis using Sankey diagrams and quantitative fuel energy-density comparisons
- Analyse conservation of mechanical energy in systems involving kinetic, gravitational potential, and elastic potential energy, identifying dissipative losses and constructing quantitative energy audits
A.4 Rigid Body Mechanics (HL Only)
- Apply torque, moment of inertia, and Newton's second law for rotation (tau = I*alpha) to solve rotational equilibrium and angular-acceleration problems for standard body geometries such as discs and rods
- Analyse conservation of angular momentum and rotational kinetic energy in spinning discs, pulleys, and rolling bodies, applying the angular-impulse relationship for impulsive torques
- Synthesise translational and rotational dynamics to solve problems where objects simultaneously translate and rotate, combining linear and angular forms of Newton's second law for rolling without slipping
A.5 Galilean and Special Relativity (HL Only)
- Recall the two postulates of special relativity and explain why Galilean velocity addition fails at relativistic speeds, citing muon-decay experimental evidence as observational confirmation
- Apply the Lorentz time-dilation and length-contraction equations to calculate proper time, coordinate time, proper length, and contracted length in relativistic observer scenarios
- Analyse spacetime (Minkowski) diagrams to represent world lines, simultaneity, and the invariant spacetime interval, and apply relativistic velocity addition for collinear motion using Lorentz transformations
2Theme B: The Particulate Nature of Matter 5 topics
B.1 Thermal Energy Transfers
- Recall specific heat capacity and latent heat definitions and apply Q = mc*deltaT and Q = mL to calculate energy exchanges during heating, cooling, and phase-change processes with appropriate SI units
- Apply Stefan-Boltzmann law (L = sigma*A*T^4) and Wien's displacement law (lambda_max * T = 2.90e-3 m*K) to calculate luminosity and peak emission wavelength for black-body and real radiating surfaces
B.2 Greenhouse Effect
- Analyse the planetary energy balance using emissivity, albedo (Earth approximately 0.30), and the solar constant to calculate Earth's equilibrium surface temperature and model atmospheric absorption effects
- Comprehend the mechanism by which CH4, H2O, CO2, and N2O absorb and re-emit infrared radiation to produce the enhanced greenhouse effect, distinguishing anthropogenic enhancement from the natural greenhouse mechanism
B.3 Gas Laws
- Apply the ideal gas equation (PV = nRT) and the individual gas laws to solve state-change problems, interpreting PV diagrams for isobaric, isovolumetric, and isothermal processes
- Analyse kinetic theory to derive gas pressure from molecular collision arguments, linking mean translational kinetic energy to absolute temperature and calculating internal energy of monatomic ideal gases
B.4 Thermodynamics (HL Only)
- Apply the first law of thermodynamics (deltaU = Q minus W) to calculate work done on or by a gas, heat transferred, and internal energy change across isovolumetric, isobaric, isothermal, and adiabatic processes
- Analyse entropy changes in reversible and irreversible processes, state the Clausius and Kelvin forms of the second law of thermodynamics, and provide real-world examples of each
- Synthesise cyclic heat-engine analysis by drawing and interpreting PV cycle diagrams, calculating thermal efficiency, and comparing achieved efficiency to the Carnot maximum (eta = 1 minus T_C over T_H)
B.5 Current and Circuits
- Apply Ohm's law, series and parallel resistance rules, and EMF-internal-resistance equation (epsilon = I(R + r)) to solve multi-component DC circuit problems including potential-difference and power calculations
- Analyse I-V characteristic curves for ohmic resistors, filament lamps, diodes, thermistors, and LDRs to identify non-linear behaviour and explain the underlying physical mechanisms for each device type
- Apply potential-divider principles to design and calculate output voltages in sensing circuits incorporating fixed resistors, thermistors, and LDRs across varying temperature and light-intensity conditions
3Theme C: Wave Behaviour 5 topics
C.1 Simple Harmonic Motion
- Recall the two conditions for simple harmonic motion and the defining equation a = negative omega-squared x, explaining the significance of the restoring force being proportional to and directed opposite displacement
- Apply SHM equations for displacement, velocity, acceleration, and period (mass-spring T = 2*pi*sqrt(m/k); simple pendulum T = 2*pi*sqrt(L/g)) using phase angle phi as the HL extension
- Analyse the interchange between kinetic and potential energy during SHM using graphical and algebraic methods, including total energy as a function of amplitude and instantaneous energy at arbitrary phase
C.2 Wave Model
- Comprehend transverse and longitudinal wave motion by sketching displacement-position and displacement-time graphs, and apply the wave equation v = f*lambda to solve for speed, frequency, and wavelength
C.3 Wave Phenomena
- Apply Snell's law (n1 sin theta1 = n2 sin theta2) to solve refraction problems, determine critical angles for total internal reflection, and explain optical fibre signal transmission
- Apply Young's double-slit formula (s = lambda*D over d) to calculate fringe spacing and evaluate constructive and destructive interference conditions in terms of path difference in wavelengths
- Analyse single-slit diffraction patterns to locate the first minimum using b sin theta = lambda, explain slit-width control of pattern spread, and calculate grating spacing via n*lambda = d*sin theta (HL)
- Synthesise the combined intensity pattern of double-slit interference modulated by single-slit diffraction to predict missing orders and sketch realistic multi-slit intensity distributions
C.4 Standing Waves and Resonance
- Comprehend how superposition of two identical counter-propagating waves produces standing waves, identifying node and antinode positions and their phase relationships relative to the driving frequency
- Apply harmonic-frequency formulas to calculate natural frequencies of vibrating strings and open and closed air columns for all standard boundary conditions and harmonic modes
- Analyse resonance and damping by interpreting amplitude-frequency response curves, distinguishing light, critical, and heavy damping in terms of energy dissipation rate and oscillatory behaviour
C.5 Doppler Effect
- Apply the Doppler effect equations for moving source and moving observer to calculate frequency and wavelength shifts for sound and electromagnetic waves in radar, ultrasound, and astronomical spectroscopy contexts
- Analyse spectral-line red-shift and blue-shift data to determine stellar radial velocities and explain the significance of Doppler measurements for inferring galactic recession and the expansion of the universe
4Theme D: Fields 4 topics
D.1 Gravitational Fields
- Apply Newton's law of universal gravitation and equate gravitational to centripetal force to solve orbital mechanics problems including Kepler's third law (T-squared proportional to r-cubed) and satellite speed
- Analyse gravitational potential energy and gravitational potential (V = negative G*M over r) to calculate escape speed, orbital binding energy, and work done moving a mass between equipotential surfaces (HL)
D.2 Electric and Magnetic Fields
- Apply Coulomb's law and the superposition principle to calculate net electric force and field strength at points due to multiple point charges, sketching radial and parallel-plate field-line diagrams
- Analyse electric potential and equipotential surfaces to calculate work done moving charges, relating electric field to rate of change of potential (E = negative deltaV over deltar) for radial and uniform fields (HL)
- Recall magnetic field patterns produced by straight wires, flat coils, and solenoids using the right-hand rule, explaining how field-line density represents field magnitude in each geometry
D.3 Motion in Electromagnetic Fields
- Apply the Lorentz force law (F = q*v*B*sin theta) to calculate magnitude and direction of magnetic force on moving charges and determine the radius of circular motion for charged particles in uniform magnetic fields
- Analyse velocity-selector and mass-spectrometer configurations using crossed electric and magnetic fields to determine charge-to-mass ratio and understand the experimental basis for charge quantisation from Millikan's experiment
- Apply the force-on-conductor formula (F = B*I*L*sin theta) and force per unit length between parallel current-carrying wires to solve problems and explain the SI definition of the ampere
D.4 Electromagnetic Induction (HL Only)
- Apply Faraday's law of electromagnetic induction (epsilon = negative delta-Phi over delta-t) to calculate induced EMF in coils and in straight conductors moving perpendicularly through uniform magnetic fields
- Analyse Lenz's law as a consequence of energy conservation to predict induced current direction in changing-flux scenarios including falling magnets, rotating coils, and eddy-current braking
- Synthesise AC generator operation by relating sinusoidal EMF output to rate of change of magnetic flux with rotation angle, and calculate peak EMF and output frequency from generator geometry and angular speed
5Theme E: Nuclear and Quantum Physics 5 topics
E.1 Structure of the Atom
- Recall Rutherford scattering experiment observations including large-angle deflection of alpha particles and the nuclear model conclusions: small, dense, positively charged nucleus surrounded by diffuse electrons
- Comprehend how discrete atomic emission and absorption line spectra provide evidence for quantised electron energy levels, and calculate photon energy and wavelength from differences between level values
- Apply the nuclear radius formula (R = R0 * A to the power of one-third) and energy conservation in head-on alpha-particle scattering to estimate nuclear density and distance of closest approach (HL extension)
- Apply the Bohr model of hydrogen to calculate quantised orbital radii, electron energies in each level, and photon frequencies for allowed transitions, including quantised angular momentum as the HL extension
E.2 Quantum Physics (HL Only)
- Comprehend the photoelectric effect, explaining why classical wave theory fails to account for threshold frequency and instantaneous emission, and define work function, threshold frequency, and stopping voltage
- Apply Einstein's photoelectric equation (E_k_max = h*f minus phi) to calculate maximum kinetic energy, stopping voltage, threshold frequency, and Planck's constant from experimental I-V and E_k-vs-f graphs
- Analyse wave-particle duality by applying de Broglie's relation (lambda = h over p) to calculate matter wavelengths and explain electron diffraction through graphite as experimental evidence of electron wave behaviour
- Analyse Compton scattering as evidence for photon momentum, applying the Compton wavelength-shift equation to calculate the change in scattered X-ray wavelength as a function of scattering angle theta
E.3 Radioactive Decay
- Recall mass defect and nuclear binding energy definitions, apply E = delta-m * c-squared with 1 u = 931.5 MeV per c-squared, and interpret the binding energy per nucleon curve to explain relative nuclear stability
- Comprehend the properties of alpha, beta-minus, beta-plus, and gamma radiation in terms of charge, mass, penetrating power, ionising ability, nuclear equation notation, and neutrino evidence from beta spectrum shape
- Apply the radioactive decay law (N = N0 * e to the power of negative lambda*t; A = lambda*N) and half-life relation (T-half = ln2 over lambda) to solve decay problems at arbitrary time intervals accounting for background (HL)
- Analyse the continuous beta-decay energy spectrum as evidence for the neutrino, distinguishing it from discrete alpha and gamma spectra as evidence for quantised nuclear energy levels and the strong nuclear force
E.4 Fission
- Comprehend the mechanism of neutron-induced fission in U-235, calculate energy released from a given fission reaction using mass defect, and explain chain-reaction conditions in terms of critical mass and neutron multiplication factor
- Analyse the roles of control rods, moderators, coolant and heat exchangers, and radiation shielding in a thermal nuclear reactor, and evaluate the safety and waste-management challenges of long-lived fission products
E.5 Fusion and Stars
- Comprehend the conditions required for sustained fusion in stellar cores including extreme temperature and pressure needed to overcome Coulomb repulsion, and identify the dominant proton-proton chain reactions in main-sequence stars
- Apply Wien's displacement law and Stefan-Boltzmann luminosity to calculate stellar surface temperature and radius from observed spectra and apparent brightness, and interpret the Hertzsprung-Russell diagram to classify spectral types and evolutionary stages
- Analyse stellar distance measurement via parallax and apply unit conversions between AU, light-year, and parsec to calculate distances and luminosities from parallax angles and apparent brightness data
Scope
Included Topics
- Theme A: Space, Time and Motion (kinematics, forces, energy, rigid body mechanics, special relativity)
- Theme B: Particulate Nature of Matter (thermal physics, greenhouse effect, gas laws, thermodynamics, circuits)
- Theme C: Wave Behaviour (SHM, wave model, interference and diffraction phenomena, standing waves, Doppler effect)
- Theme D: Fields (gravitational, electric and magnetic fields, charged-particle motion, electromagnetic induction)
- Theme E: Nuclear and Quantum Physics (atomic structure, quantum physics, radioactive decay, fission, fusion and stellar physics)
- HL-only topics: A.4 Rigid Body Mechanics, A.5 Special Relativity, B.4 Thermodynamics, D.4 Induction, E.2 Quantum Physics
- HL extensions within shared topics: gravitational and electric potential, diffraction gratings, Bohr model, decay constant
- Experimental and data-analysis skills: uncertainty propagation, graphical analysis, SI units
- Scientific Investigation (internal assessment): student-designed experimental inquiry
- Assessment objectives AO1 (knowledge), AO2 (application), AO3 (analysis/evaluation), AO4 (experimental skills)
Not Covered
- IB Physics Standard Level-only assessments and grade boundaries
- IB Chemistry, Biology, and Environmental Systems and Societies content
- Calculus-based university physics beyond IB scope (e.g. Maxwell equations in differential form, Lagrangian mechanics)
- Engineering Physics optional topic (retired in 2025 syllabus restructure)
- Imaging optional topic (retired in 2025 syllabus restructure)
- Particle physics beyond the Standard Model and quark-level detail not in the IB guide
Official Exam Page
Learn more at International Baccalaureate