IB Physics Syllabus Checklist

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This Interactive syllabus checklist for IB Physics is broken down by topics, then subtopics. Your progress is saved site-wide and you can update it as you move throughout the IB Physics syllabus.

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1: Space, Time & Motion

2: The Particulate Nature of Matter

3: Wave Behaviour

4: Fields

5: Nuclear & Quantum Physics

1 - Space, Time & Motion

Mark Complete

Master IB Physics Topic 1: Space, Time & Motion. Explore classical mechanics with detailed study notes on kinematics, Newton's laws of motion, forces, momentum, work, and mechanical energy. Elevate your HL physics knowledge by mastering rigid body mechanics, torque, and Galilean and special relativity.

Subtopic

Understanding

A1: Kinematics & motion

Recall that the motion of bodies through space and time can be described and analysed in terms of position, velocity, and acceleration.

Recall that velocity is the rate of change of position, and acceleration is the rate of change of velocity.

Understand that the change in position is the displacement.

Recall the difference between distance and displacement.

Recall the difference between instantaneous and average values of velocity, speed and acceleration, and how to determine them.

Understand and use the equations of motion for solving problems with uniformly accelerated motion as given by:

s = $\frac{u + v}{2}t$
v = u + at
s = u t + $\frac{1}{2}$ at²
v² = u² + 2as

Understand motion with uniform and non-uniform acceleration.

Understand the behaviour of projectiles in the absence of fluid resistance, and the application of the equations of motion resolved into vertical and horizontal components.

Recall the qualitative effect of fluid resistance on projectiles, including time of flight, trajectory, velocity, acceleration, range and terminal speed.

A2: Forces & momentum

Recall Newton’s three laws of motion and understand that forces are interactions between bodies.

Understand that forces acting on a body can be represented in a free-body diagram and that free-body diagrams can be analysed to find the resultant force on a system.

Understand the nature and use of the following contact forces:

Normal force F_N.
Surface frictional force F_f acting in a direction parallel to the plane of contact between a body and a surface, on a stationary body as given by F_f ≤ μ_sF_N or a body in motion as given by
F_f = μ_dF_N.
Tension.
Elastic restoring force F_H following Hooke’s law as given by F_H = –kx.
Viscous drag force F_d acting on a small sphere opposing its motion through a fluid as given by F_d = 6πηrv.
Buoyancy F_b acting on a body due to the displacement of the fluid as given by F_b = ρVg.

Understand the nature and use of the following field forces:

Gravitational force F_g is the weight of the body and calculated by F_g = mg.
Electric force F_e.
Magnetic force F_m.

Recall that linear momentum, as given by p = mv, remains constant unless the system is acted upon by a resultant external force.

Understand that a resultant external force applied to a system constitutes an impulse J as given by J = FΔt where F is the average resultant force and Δt is the time of contact.

Understand that the applied external impulse equals the change in momentum of the system.

Understand that Newton’s second law in the form F = ma assumes mass is constant whereas F = Δp allows for situations where mass is changing.

Recall the elastic and inelastic collisions of two bodies and understand explosions, including energy considerations in elastic collisions, inelastic collisions, and explosions.

10:

Understand that bodies moving along a circular trajectory at a constant speed experience an acceleration that is directed radially towards the centre of the circle—known as a centripetal acceleration as given by: a = $\frac{v^{2}}{r}$ = ω²r= $\frac{4π^{2}r}{T^{2}}$

11:

Understand that circular motion is caused by a centripetal force acting perpendicular to the velocity.

12:

Understand that a centripetal force causes the body to change direction even if its magnitude of velocity may remain constant.

13:

Understand that the motion along a circular trajectory can be described in terms of the angular velocity ω which is related to the linear speed v by the equation as given by v = $\frac{2πr}{T}$ = ωr.

A3: Work, energy sources & power

Recall the principle of the conservation of energy and understand that work done by a force is equivalent to a transfer of energy.

Understand that energy transfers can be represented on a Sankey diagram.

Understand that work W done on a body by a constant force depends on the component of the force along the line of displacement as given by W = Fs cos θ.

Recall that work done by the resultant force on a system is equal to the change in the energy of the system.

Recall that mechanical energy is the sum of kinetic energy, gravitational potential energy and elastic potential energy, and that in the absence of frictional, resistive forces, the total mechanical energy of a system is conserved.

Understand that if mechanical energy is conserved, work is the amount of energy transformed between different forms of mechanical energy in a system, such as:

the kinetic energy of translational motion as given by: E_k = $\frac{1}{2}$ mv² = p² ÷ 2m.
the gravitational potential energy, when close to the surface of the Earth as given by: ΔE_p = mgΔh
the elastic potential energy as given by: E_H = $\frac{1}{2}$ k(Δx)²

Understand that power developed P is the rate of work done, or the rate of energy transfer, as given by P = $\frac{\Delta W}{\Delta t}$ = Fv

Recall efficiency η in terms of energy transfer or power as given by η = $\frac{E_{output}}{E_{input}}= \frac{P_{output}}{P_{input}}$

Understand energy density of fuel sources.

A4: Rigid body mechanics (HL)

Recall the torque τ of a force about an axis as given by τ = Fr sin θ.

Understand that bodies in rotational equilibrium have a resultant torque of zero and that an unbalanced torque applied to an extended, rigid body will cause angular acceleration.

Understand that the rotation of a body can be described in terms of angular displacement, angular velocity and angular acceleration.

Understand that equations of motion for uniform angular acceleration can be used to predict the body’s angular position θ, angular displacement Δθ, angular speed ω and angular acceleration $\alpha$ , as given by:

Δθ = $\frac{\omega_f + \omega_i}{2}t$
ω_f = ω_i + αt
Δθ = ω_it + $\frac{1}{2}$ αt²
$\omega_f^2$ = $\omega_i^2$ + 2αΔθ

Understand that the moment of inertia I depends on the distribution of mass of an extended body about an axis of rotation.

Recall the moment of inertia for a system of point masses as given by I = Σmr².

Recall Newton’s second law for rotation as given by τ = Iα where τ is the average torque.

Understand that an extended body rotating with an angular speed has an angular momentum L as given by: L = Iω

Understand that angular momentum remains constant unless the body is acted upon by a resultant torque and that the action of a resultant torque constitutes an angular impulse ΔL as given by: ΔL = τΔt = Δ(Iω)

10:

Understand the kinetic energy of rotational motion as given by E_k = $\frac{1}{2}$ Iω² = $\frac{L^2}{2I}$ .

A5: Galilean & special relativity (HL)

Understand reference frames and that Newton's laws of motion are the same in all inertial reference frames and this is known as Galilean relativity.

Recall that in Galilean relativity the position x′ and time t′ of an event are given by x′ = x – vt and t′ = t.

Recall that Galilean transformation equations lead to the velocity addition equation as given by u′ = u – v.

Understand the two postulates of special relativity.

Understand that the postulates of special relativity lead to the Lorentz transformation equations for the coordinates of an event in two inertial reference frames as given by:

x′ = γ(x – vt)
t′ = γ(t – $\frac{vx}{c^2}$ )

Understand that Lorentz transformation equations lead to the relativistic velocity addition equation as given by: u′ = $\frac{u-v}{1 - \frac{uv}{c^2}}$

Understand that the space–time interval Δs between two events is an invariant quantity as given by (Δs)² = (cΔt)²– (Δx)².

Recall proper time interval and proper length.

Understand time dilation as given by: Δt = γΔt₀.

10:

Understand length contraction as given by: L = L₀ ÷ γ

11:

Understand the relativity of simultaneity.

12:

Interpret space–time diagrams.

13:

Understand that the angle between the world line of a moving particle and the time axis on a space–time diagram is related to the particle’s speed as given by tan θ = v ÷ c.

14:

Recall that muon decay experiments provide experimental evidence for time dilation and length contraction.

2 - The Particulate Nature of Matter

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Excel in IB Physics Topic 2: The Particulate Nature of Matter. Discover the thermal properties of matter with comprehensive guides on thermal energy transfers, the kinetic theory of gases, and the global greenhouse effect. Master advanced thermodynamics and explore the fundamentals of electric fields, currents, and circuits.

Subtopic

Understanding

B1: Thermal energy transfers

Understand molecular theory in solids, liquids and gases.

Recall density ρ as given by: ρ = mV

Understand that Kelvin and Celsius scales are used to express temperature and that the change in temperature of a system is the same when expressed with the Kelvin or Celsius scales.

Understand that Kelvin temperature is a measure of the average kinetic energy of particles as given by $\overline{E_k} = \frac{3}{2}k_BT$ .

Understand that the internal energy of a system is the total intermolecular potential energy arising from the forces between the molecules plus the total random kinetic energy of the molecules arising from their random motion.

Understand that temperature difference determines the direction of the resultant thermal energy transfer between bodies.

Understand that a phase change represents a change in particle behaviour arising from a change in energy at constant temperature.

Understand that quantitative analysis of thermal energy transfers (Q) with the use of specific heat capacity (c) and specific latent heat of fusion and vaporization of substances (L) as given by Q = mcΔT and Q = mL.

Understand that conduction, convection and thermal radiation are the primary mechanisms for thermal energy transfer and explain conduction in terms of the difference in the kinetic energy of particles.

10:

Understand quantitative analysis of rate of thermal energy transfer by conduction in terms of the type of material and cross-sectional area of the material and the temperature gradient as given by: $\frac{\Delta Q}{\Delta t}=kA\frac{\Delta T}{\Delta x}$

11:

Understand the qualitative description of thermal energy transferred by convection due to fluid density differences.

12:

Understand the quantitative analysis of energy transferred by radiation as a result of the emission of electromagnetic waves from the surface of a body, which in the case of a black body can be modelled by the Stefan-Boltzmann law as given by: L = σAT⁴.

13:

Recall the concept of apparent brightness (b) and luminosity (L) of a body as given by: b = L ÷ 4πd².

14:

Understand the emission spectrum of a black body and the determination of the temperature of the body using Wien’s displacement law as given by: λ_maxT = 2.9 ×10⁻³mK where λ_maxis the peak wavelength emitted.

Recall the solar constant S.

B2: The greenhouse effect

Recall the conservation of energy.

Recall emissivity 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 as given by emissivity = power radiated per unit area ÷ σT⁴

Recall albedo as a measure of the average energy reflected off a macroscopic system as given by: albedo = total scattered power ÷ total incident power

Understand that Earth’s albedo varies daily and is dependent on cloud formations and latitude.

Understand that the incoming radiative power is dependent on the projected surface of a planet along the direction of the path of the rays, resulting in a mean value of the incoming intensity being S ÷ 4.

Recall methane CH₄, water vapour H₂O, carbon dioxide CO₂, and nitrous oxide N₂O, as the main greenhouse gases. Understand that each of these has origins that are both natural and created by human activity.

Understand the absorption of infrared radiation by the main greenhouse gases in terms of the molecular energy levels and the subsequent emission of radiation in all directions.

Understand that the greenhouse effect can be explained in terms of both a resonance model and molecular energy levels.

10:

Recall that the augmentation of the greenhouse effect due to human activities is known as the enhanced greenhouse effect.

B3: Gas laws

Define pressure as given by: P = F ÷ A.

Understand that the amount of substance n is given by n = N ÷ N_A.

Understand that ideal gases are described in terms of the kinetic theory and constitute a modelled system used to approximate the behaviour of real gases.

Understand that the ideal gas law equation can be derived from the empirical gas laws for constant pressure, constant volume and constant temperature as given by PV ÷ T = constant.

Recall the equations governing the behaviour of ideal gases as given by: PV = Nk_BT and PV = nRT.

Understand that the change in momentum of particles due to collisions with a given surface gives rise to pressure in gases and, from that analysis, pressure is related to the average translational speed of molecules as given by: P = $\frac{1}{3}$ ρv².

Understand the relationship between the internal energy U of an ideal monatomic gas and the number of molecules or amount of substance as given by U = $\frac{3}{2}$ Nk_BT or U = $\frac{3}{2}$ RnT.

Understand the temperature, pressure and density conditions under which an ideal gas is a good approximation of a real gas.

B4: Thermodynamics (HL)

Understand the first law of thermodynamics, as given by Q = ΔU + W, results from the application of conservation of energy to a closed system and relates the internal energy of a system to the transfer of energy as heat and as work.

Understand that the work done by or on a closed system as given by W = PΔV when its boundaries are changed can be described in terms of pressure and changes of volume of the system.

Understand that the change in internal energy as given by ΔU = $\frac{3}{2}$ Nk_BΔT = $\frac{3}{2}$ nRΔT of a system is related to the change of its temperature.

Recall that entropy S is a thermodynamic quantity that relates to the degree of disorder of the particles in a system.

Understand that entropy can be determined in terms of macroscopic quantities, such as thermal energy and temperature, as given by: ΔS = ΔQ ÷ T, and also in terms of the properties of individual particles of the system as given by: S = k_BlnΩ.

Recall that the second law of thermodynamics refers to the change in entropy of an isolated system and sets constraints on possible physical processes and on the overall evolution of the system.

Recall that processes in real isolated systems are almost always irreversible and consequently the entropy of a real isolated system always increases.

Understand that the entropy of a non-isolated system can decrease locally, but this is compensated by an equal or greater increase of the entropy of the surroundings.

Understand that isovolumetric, isobaric, isothermal and adiabatic processes are obtained by keeping one variable fixed.

10:

Understand that adiabatic processes in monatomic ideal gases can be modelled by the equation as given by $PV^{\frac{5}{3}}$ = constant

11:

Recall that cyclic gas processes are used to run heat engines.

12:

Understand that a heat engine can respond to different cycles and is characterized by its efficiency as given by:

η = useful work ÷ input energy.

13:

Recall that the Carnot cycle sets a limit for the efficiency of a heat engine at the temperatures of its heat reservoirs as given by η_Carnot = 1 - $\frac{T_c}{T_h}$

B5: Current & circuits

Recall that cells provide a source of emf, chemical cells and solar cells are the energy source in circuits, and that circuit diagrams represent the arrangement of components in a circuit.

Define direct current (dc) I as a flow of charge carriers as given by I = Δ_q÷ Δ_t.

Understand that the electric potential difference V is the work done per unit charge on moving a positive charge between two points along the path of the current as given by V = W ÷ q.

Understand the properties of electrical conductors and insulators in terms of mobility of charge carriers.

Recall electric resistance, as given by R = V ÷ I, and its origin.

Understand resistivity as given by: ρ = RA ÷ L

Understand Ohm’s law and the ohmic and non-ohmic behaviour of electrical conductors, including the heating effect of resistors.

Understand electrical power P dissipated by a resistor as given by P = IV = I²R = V² ÷ R.

Recall the combinations of resistors in series and parallel circuits.

10:

Understand that electric cells are characterized by their emf ε and internal resistance r as given by ε = I(R + r).

11:

Recall that resistors can have variable resistance.

3 - Wave Behaviour

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Ace IB Physics Topic 3: Wave Behaviour. Dive into the mechanics of waves with in-depth notes on simple harmonic motion, transverse and longitudinal wave models, and standing waves. Master essential wave phenomena including reflection, refraction, single-slit diffraction, resonance, and the Doppler effect for both moving observers and sources.

Subtopic

Understanding

C1: Simple harmonics

Understsand conditions that lead to simple harmonic motion.

Recall the defining equation of simple harmonic motion as given by: a = –ω²x.

Recall that a particle undergoing simple harmonic motion can be described using time period T, frequency ƒ, angular frequency ω, amplitude, equilibrium position, and displacement.

Understand the time period in terms of frequency of oscillation and angular frequency as given by: T = $\frac{1}{f}$ = $\frac{2\pi}{\omega}$

Recall the time period of a mass–spring system as given by: T = 2π $\sqrt{m \div k}$ .

Recall that the time period of a simple pendulum is given by: T = 2π $\sqrt{l ÷ g}$ .

Understand a qualitative approach to energy changes during one cycle of an oscillation.

C1: Further simple harmonics (HL)

Understand that a particle undergoing simple harmonic motion can be described using phase angle.

Recall and utilise various equations for simple harmonic motion, including:

x = x₀sin(ωt + φ)
v = ωx₀cos(ωt + φ)
v = ± ω $\sqrt{x_0^2 x^2}$
E_T = $\frac{1}{2}$ mω² $x_0^2$
E_p = $\frac{1}{2}$ mω²x².

C2: Wave models

Understand transverse and longitudinal travelling waves.

Recall that wavelength λ, frequency ƒ, time period T, and wave speed v are applied to wave motion as given by:

v = ƒλ = λ ÷ T.

Understand the nature of sound and electromagnetic waves.

Understand the differences between mechanical waves and electromagnetic waves.

C3: Wave phenomena

Understand that waves travelling in two and three dimensions can be described through the concepts of wavefronts and rays.

Understand wave behaviour at boundaries in terms of reflection, refraction and transmission.

Describe wave diffraction around a body and through an aperture.

Draw and interpret wavefront-ray diagrams showing refraction and diffraction.

Recall Snell’s law, the critical angle and total internal reflection.

Understand Snell’s law as given by: $\frac{n_1}{n_2}=\frac{sin\theta_2}{sin\theta_1}=\frac{v_2}{v_1}$ .

Understand superposition of waves and wave pulses.

Recall that double-source interference requires coherent sources.

Recall the condition for constructive interference: path difference = nλ, and recall the condition for destructive interference: path difference = (n + $\frac{1}{2}$ )λ.

10:

Understand Young’s double-slit interference as given by: s = λD ÷ d.

C3: Further wave phenomena (HL)

Recall single-slit diffraction including intensity patterns as given by θ = b ÷ λ.

Understand that the single-slit pattern modulates the double slit interference pattern.

Understand interference patterns from multiple slits and diffraction gratings as given by: nλ = d sinθ.

C4: Standing waves & resonance

Understand the nature and formation of standing waves in terms of superposition of two identical waves travelling in opposite directions.

Understand nodes and antinodes, relative amplitude and phase difference of points along a standing wave.

Understand standing waves patterns in strings and pipes.

Recall the nature of resonance including natural frequency and amplitude of oscillation based on driving frequency.

Understand the effect of damping on the maximum amplitude and resonant frequency of oscillation, and the effects of light, critical and heavy damping on the system.

C5: Doppler effect

Understand the nature of the Doppler effect for sound waves and electromagnetic waves.

Understand the representation of the Doppler effect in terms of wavefront diagrams when either the source or the observer is moving.

Understand the relative change in frequency or wavelength observed for a light wave due to the Doppler effect where the speed of light is much larger than the relative speed between the source and the observer as given by:

Δƒ ÷ f = Δλ ÷ λ ≈ v ÷ c.

Understand that shifts in spectral lines provide information about the motion of bodies like stars and galaxies in space.

C5: Further Doppler effects (HL)

Understand the observed frequency for sound waves and mechanical waves due to the Doppler effect as given by:

moving source ƒ′ = $f\left ( \frac{v}{v \pm u_s} \right )$ .
moving observer ƒ′ = $f\left ( \frac{v \pm u_o}{v} \right )$ .

4 - Fields

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Unlock IB Physics Topic 4: Fields. Understand the invisible forces of the universe with comprehensive study materials on gravitational and electromagnetic fields. Learn to calculate orbital motion, escape speeds, and electric potentials, and master the concepts of electromagnetic motion, moving charges, and electromagnetic induction for your IB exams.

Subtopic

Understanding

D1: Gravitational fields

Recall Kepler’s three laws of orbital motion.

Undertand Newton's universal law of gravitation as given by: F = G $\frac{m_1 m_2}{r_2}$ for bodies treated as point masses.

Recall the conditions under which extended bodies can be treated as point masses.

Understand that gravitational field strength g at a point is the force per unit mass experienced by a small point mass at that point is given by: $g = \frac{F}{m} = G\frac{M}{r_2}$ .

Draw and interpret gravitational field lines.

D1: Further gravitational fields (HL)

Understand that the gravitational potential energy Ep of a system is the work done to assemble the system from infinite separation of the components of the system.

Recall that the gravitational potential energy for a two-body system is given by: E_p = –G $\frac{m_1 m_2}{r}$ .

Recall that the gravitational potential V_g at a point is the work done per unit mass in bringing a mass from infinity to that point is given by: V_g= –G(M ÷ r).

Understand the gravitational field strength g as the gravitational potential gradient as given by: g = - $\frac{\Delta V_g}{\Delta r}$ .

Understand the work done in moving a mass m in a gravitational field as given by W = mΔV_g.

Understand equipotential surfaces for gravitational fields.

Understand the relationship between equipotential surfaces and gravitational field lines.

Recall and calculate the escape speed v_esc at any point in a gravitational field as given by v_esc = $\sqrt{\frac{2GM}{r}}$ .

Recall and calculate the orbital speed vorbital of a body orbiting a large mass as given by v_orbital = $\sqrt{\frac{GM}{r}}$ .

10:

Understand the qualitative effect of a small viscous drag force due to the atmosphere on the height and speed of an orbiting body.

D2: Electromagnetic fields

Understand the direction of forces between the two types of electric charge.

Understand Coulomb’s law as given by: F = k $\frac{q_1 q_2}{r^2}$ for charged bodies treated as point charges where k = $\frac{1}{4\pi \epsilon_0}$ .

Recall the conservation of electric charge.

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

Understand that the electric charge can be transferred between bodies using friction, electrostatic induction and by contact, including the role of grounding (earthing).

Recall the electric field strength as given by: E = F ÷ q.

Understand electric field lines and the relationship between field line density and field strength.

Understand the uniform electric field strength between parallel plates as given by: E = V ÷ d.

Understand magnetic field lines.

D2: Further electromagnetic fields (HL)

Understand the electric potential energy E_p in terms of work done to assemble the system from infinite separation.

Understand the electric potential energy for a system of two charged bodies as given by: E_p = k $\frac{q_1 q_2}{r}$ .

Understand that the electric potential is a scalar quantity with zero defined at infinity.

Understand that the electric potential V_e at a point is the work done per unit charge to bring a test charge from infinity to that point as given by V_e= kQ ÷ r.

Understand the electric field strength E as the electric potential gradient as given by: E = - $\frac{\Delta V_e}{\Delta r}$ .

Understand the work done in moving a charge q in an electric field as given by W = qΔV_e.

Understand equipotential surfaces for electric fields.

Recall the relationship between equipotential surfaces and electric field lines.

D3: Electromagnetic motion

Understand the motion of a charged particle in a uniform electric and magnetic field.

Understand the motion of a charged particle in perpendicularly orientated uniform electric and magnetic fields.

Understand the magnitude and direction of the force on a charge moving in a magnetic field as given by: F = qvB sinθ

Understand the magnitude and direction of the force on a current-carrying conductor in a magnetic field as given by: F = BΙL sin θ.

Understand the force per unit length between parallel wires as given by: $\frac{F}{L}=\mu_0\frac{I_1 I_2}{2\pi r}$ .

D4: Induction (HL)

Recall magnetic flux Φ as given by Φ = BA cosθ.

Understand that a time-changing magnetic flux induces an emf ε as given by Faraday’s law of induction: ε = −N $\frac{\Delta \Phi }{\Delta t}$ .

Understand that a uniform magnetic field induces an emf in a straight conductor moving perpendicularly to it as given by: ε = BvL.

Understand that the direction of induced emf is determined by Lenz’s law and is a consequence of energy conservation.

Understand that a uniform magnetic field induces a sinusoidal varying emf in a coil rotating within it.

Understand the effect on induced emf caused by changing the frequency of rotation.

5 - Nuclear & Quantum Physics

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Conquer IB Physics Topic 5: Nuclear & Quantum Physics. Explore the subatomic world with detailed notes on atomic structure, nuclear energy levels, and wave-particle duality. Master the mathematical processes of radioactive decay and half-life calculations, alongside the mechanisms of nuclear fission and the role of fusion in stellar evolution.

Subtopic

Understanding

E1: Atomic structure

Understand the Geiger–Marsden–Rutherford experiment and the discovery of the nucleus.

Understand nuclear notation $_{Z}^{A}\textrm{X}$ .

Understand that emission and absorption spectra provide evidence for discrete atomic energy levels.

Understand that photons are emitted and absorbed during atomic transitions.

Understand that the frequency of the photon released during an atomic transition depends on the difference in energy level as given by E = hƒ.

Understand that emission and absorption spectra provide information on the chemical composition.

E1: Further atomic structure (HL)

Recall the relationship between the radius and the nucleon number for a nucleus as given by: R = R₀A^1/3 and implications for nuclear densities.

Describe deviations from Rutherford scattering at high energies.

Understand the distance of closest approach in head-on scattering experiments.

Understand the discrete energy levels in the Bohr model for hydrogen, as given by: E = - $\frac{13.6}{n^2}$ eV.

Understand that the existence of quantized energy and orbits arise from the quantization of angular momentum in the Bohr model for hydrogen as given by: mvr = $\frac{nh}{2\pi}$ .

E2: Quantum physics (HL)

Recall that the photoelectric effect as evidence of the particle nature of light.

Understand that photons of a certain frequency, known as the threshold frequency, are required to release photoelectrons from the metal.

Understand Einstein’s explanation using the work function and the maximum kinetic energy of the photoelectrons as given by E_max = hƒ – Φ where Φ is the work function of the metal.

Recall that diffraction of particles as evidence of the wave nature of matter.

Understand that matter exhibits wave–particle duality.

Understand the de Broglie wavelength for particles as given by: λ = h ÷ p.

Recall Compton scattering of light by electrons as additional evidence of the particle nature of light.

Understand that photons scatter off electrons with increased wavelength.

Understand the shift in photon wavelength after scattering off an electron as given by: λ_f- λ_i = Δλ = $\frac{h}{m_e c}$ (1–cos θ).

E3: Radioactive decay

Understand the concept of isotopes.

Understand nuclear binding energy and mass defect.

Understand the variation of the binding energy per nucleon with nucleon number.

Understand the mass-energy equivalence as given by: E = mc² in nuclear reactions.

Understand the existence of the strong nuclear force, a short-range, attractive force between nucleons.

Appreciate the random and spontaneous nature of radioactive decay.

Understand the changes in the state of the nucleus following alpha, beta and gamma radioactive decay.

Recall the radioactive decay equations involving α, β⁻, β⁺, and γ.

Appreciate the existence of neutrinos ν and antineutrinos $\overline{v}$ .

10:

Describe the penetration and ionizing ability of alpha particles, beta particles and gamma rays.

11:

Understand the activity, count rate and half-life in radioactive decay.

12:

Recall the changes in activity and count rate during radioactive decay using integer values of half-life.

13:

Understand the effect of background radiation on count rate.

E3: Further radioactive decay (HL)

Recall the evidence for the strong nuclear force.

Understand the role of the ratio of neutrons to protons for the stability of nuclides.

Recall the approximate constancy of binding energy curve above a nucleon number of 60.

Understand that the spectrum of alpha and gamma radiations provides evidence for discrete nuclear energy levels.

Understand the continuous spectrum of beta decay as evidence for the neutrino.

Recall the decay constant λ and the radioactive decay law as given by: N = N₀e⁻^λt.

Understand that the decay constant approximates the probability of decay in unit time only in the limit of sufficiently small λt.

Understand the activity as the rate of decay as given by: A = λN = λN₀e⁻^λt.

Understand the relationship between half-life and the decay constant as given by T_1/2 = ln2 ÷ λ.

E4: Fission

Understand that energy is released in spontaneous and neutron-induced fission.

Understand the role of chain reactions in nuclear fission reactions.

Recall the role of control rods, moderators, heat exchangers and shielding in a nuclear power plant.

Understand the properties of the products of nuclear fission and their management.

E5: Fusion & stars

Understand that the stability of stars relies on an equilibrium between outward radiation pressure and inward gravitational forces.

Recall that fusion is a source of energy in stars.

Describe the conditions leading to fusion in stars in terms of density and temperature.

Understand the effect of stellar mass on the evolution of a star.

Understand the main regions of the Hertzsprung–Russell (HR) diagram and how to describe the main properties of stars in these regions.

Understand the use of stellar parallax as a method to determine the distance d to celestial bodies as given by: d(parsec) = 1 ÷ p(arc‐second).

Understand how to determine stellar radii.

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