IB Physics Interactive Checklist
Topic A: Space, Time and Motion
A.1 Kinematics
Define and differentiate displacement, velocity, and acceleration
Compare and contrast distance and displacement with examples
Determine instantaneous and average values for velocity, speed, and acceleration
Identify cases of uniform and non-uniform acceleration
Understand that motion equations apply only in cases of constant acceleration
Apply kinematic equations to solve motion-related problems
Explain the concept of a projectile and break its motion into horizontal and vertical components
Analyze projectile motion for different launch angles, assuming negligible air resistance
Discuss how air resistance influences the trajectory, flight time, velocity, acceleration, and terminal velocity
A.2 Forces and Momentum
List and explain Newton’s three laws of motion
Apply Newton’s First Law to solve translational equilibrium problems
Determine action-reaction force pairs based on Newton’s Third Law
Explain how forces act as interactions between objects
Construct and analyze free-body diagrams to determine net force in one and two dimensions
Identify and describe contact forces, including normal, frictional, elastic, drag, and buoyant forces
Differentiate between field forces such as gravitational, electric, and magnetic forces
Define linear momentum and recognize that it remains conserved unless acted upon by an external force
Define impulse as an external force applied over time and relate it to the change in momentum
Derive Newton’s Second Law from the relationship between net force and the rate of momentum change
Use momentum and impulse equations to solve collision and explosion problems (1D for SL, 2D for HL)
Distinguish between elastic and inelastic collisions and understand the principles behind explosions
Explain that objects in circular motion maintain a constant speed while experiencing centripetal acceleration toward the center
Illustrate with a vector diagram how acceleration in uniform circular motion always points toward the center
Identify the directions of velocity, acceleration, and force vectors for an object in circular motion
Analyze and solve problems involving centripetal force, acceleration, period, frequency, angular displacement, linear velocity, and angular velocity
A.3 Work, Energy and Power
State the law of conservation of energy
Recognize that work done by a force corresponds to energy transfer within a system
Draw and interpret Sankey diagrams to analyze energy transfers
Calculate work done using \( W = F s \cos\theta \), including cases involving resistive forces and non-parallel force and displacement
Understand that mechanical energy is the sum of kinetic, gravitational potential, and elastic potential energy in the absence of friction, and apply this to problem-solving
Use appropriate equations to solve problems related to work and energy transfer in systems where mechanical energy is conserved
Define power as the rate at which work is done or energy is transferred, and solve problems involving power
Express efficiency as a ratio of useful energy output to total energy input and apply it to solve efficiency-related problems
Define energy density of a fuel source and apply it to relevant calculations
A.4 Rigid Body Mechanics (HL)
Describe the torque τ of a force about an axis as given by τ = Fr sin θ
State that bodies in rotational equilibrium have a resultant torque of zero
State that an unbalanced torque applied to an extended, rigid body will cause angular acceleration
Describe the rotation of a body in terms of angular displacement, angular velocity and angular acceleration
Calculate the position θ, angular displacement Δθ, angular speed ω and angular acceleration α of an object using the equations of motion (SUVAT Equivalents) for uniform angular acceleration.
Define and perform calculations using the moment of inertia, I
Calculate using Newton’s second law for rotation as given by τ = Iα where τ is the average torque.
Calculate angular momentum, L for an extended body rotating with an angular speed
Understand that angular momentum remains constant (i.e. ΔL=0) unless the body is acted upon by a resultant torque
Explain how the action of a resultant torque will cause angular impulse
Calculate the kinetic energy of rotational motion
A.5 Galilean and Special Relativity (HL)
Define a reference frame and understand the concept of an inertial reference frame
Explain that Newton's laws of motion are consistent in all internal reference frames, a concept known as Galilean relativity
Understand that in Galilean relativity, the position x' and time t' of an event are given by x'=x-vt and t'=t
Describe velocity addition for a Galilean transformation as given by u' = u - v
Memorise the two postulates of special relativity
Calculate the motion of a particle at high speeds using the Lorentz transformation equations for the coordinates of an event in two inertial reference frames
Solve problems using the relativistic velocity addition equation
Calculate the invariant quantity of the space-time interval between two events
Define what is meant by proper time interval and proper length
Solve problems involving time dilation
Compute length dilation
Explain the concept of relativity of simultaneity
Interpret space-time diagrams to represent the motion of particles
Calculate the angle between the world line of a moving particle and the time axis on a space-time diagram
Interpret muon decay experiments to demonstrate evidence for time dilation and length contraction
Topic B: The Particulate Nature of Matter
B.1 Thermal Energy Transfers
Explain the physical differences between the solid, liquid and gaseous phases in terms of molecular structure and particle motion (Note: be familiar with the terms melting, freezing, evaporating, boiling and condensing, and be able to describe each in terms of the changes in molecular potential and random kinetic energies of molecules)
Define density using the equation ρ=m/V
Use Kelvin and Celsius temperature scales and convert between them (T/K = t/°C + 273)
Understand that the average kinetic energy of ideal gas molecules is directly proportional to the temperature (in kelvin) of the gas
Understand that internal energy is taken to be the total intermolecular potential energy and the total random kinetic energy of the molecules
Know that temperature difference depends on thermal energy transfer between bodies from hot to cold
Explain in terms of molecular behaviour why temperature does not change during a phase change
Define and solve problems with specific heat capacity and specific latent heat of fusion and vaporization
Describe on a molecular level how conduction, convection and radiation are mechanisms for thermal energy transfer
Perform calculations on the rate of kinetic energy transfer in conduction
Solve problems involving the Stefan-Boltzmann Law and Wien's displacement law
Define luminosity and apparent brightness AND solve problems involving luminosity, apparent brightness and distance
B.2 Greenhouse Effect
State the conservation of energy
Define and solve problems using emissivity and albedo
Know that the Earth's average albedo is 0.3; however, this varies daily depending on cloud formation and latitude
Define the Solar Constant, S, and explain why effective incident power on the Earth’s surface is S/4
Calculate equilibrium temperature of a body using energy balance between incoming and outgoing radiation intensity, including albedo, emissivity, and solar or other constants
Know that the four greenhouse gases are CH₄, H₂O, CO₂ and N₂O, and that each gas is both man-made and naturally occurring in the atmosphere
Explain how the Earth radiates thermal radiation as a black body, which is absorbed by greenhouse gases, and then scattered in all directions (molecular energy levels), and subsequently heats up the Earth's surface
Define enhanced greenhouse effect as an augmentation of the naturally occurring greenhouse effect due to human activities
State that burning of fossil fuels is a primary cause of the enhanced greenhouse effect
Explain how the main greenhouse gases cause enhanced greenhouse effect by referring to molecular energy levels, absorbed infrared radiation, resonance, and the subsequent emission of radiation in all directions
Calculate energy balance problems that include energy exchanged between the surface and the atmosphere of a body
B.3 Gas Laws
State the assumptions of the kinetic theory of ideal gases, understanding this modelled system is used to approximate the behaviour of real gases
Understand that a real gas approximates to an ideal gas at conditions of low pressure, moderate temperature and low density
Define and solve problems using pressure as P=F/A
Define the amount of substance, n
Solve problems using the equation of state for an ideal gas and gas laws
Know that gas laws are limited to constant volume, constant temperature, constant pressure and the ideal gas law
Explain how the ideal gas law is derived empirically from gas laws
Sketch and interpret changes of state of an ideal gas on pressure-volume diagrams
Calculate changes in pressure due to collisions with the walls of the container
Calculate internal energy, U of an ideal monatomic gas
B.4 Thermodynamics (HL)
Describe the first law of thermodynamics as a statement of conservation of energy and solve problems using the first law
Define the work done by or on a closed system
Calculate the change in internal energy for a system undergoing a change in temperature or volume
Describe the second law of thermodynamics in Celsius form, Kelvin form and as a consequence of entropy
Solve problems involving entropy changes
Understand isovolumetric, isobaric, isothermal and adiabatic processes
Solve problems for adiabatic processes for monatomic gases
Sketch and interpret cyclic processes which are used to run heat engines (Only graphical analysis will be required for determination of work done on a pV diagram when pressure is not constant)
Solve problems involving thermal efficiency
Define the Carnot cycle as a theoretical heat engine cycle that has the maximum possible efficiency of any heat engine and calculate the efficiency of a Carnot cycle
B.5 Current and Circuits
Define emf and electric potential difference, V
Describe how chemical cells and solar cells are energy sources in circuits
Be comfortable drawing circuit diagrams with a variety of components
Recognise current as the rate of flow of charge
Know that charge carriers within a metal are electrons, but they may be ions in other materials
Describe an ideal ammeter, an ideal voltmeter, and understand that most practical meters do not meet these requirements
Explain origin of electrical resistance and define resistance as R=V/I
State Ohm's Law
Know the I/V characteristics of ohmic conductors (metal wire at a constant temperature) and non-ohmic conductors (filament lamp and diode)
Solve problems involving potential difference, current, charge, power, resistivity and resistance in both series and parallel circuits
Describe Internal Resistance in cells and solve problems using ε = I(R+r)
Describe how resistance varies in thermistors, light-dependent resistors (LDR) and potentiometers
Describe practical uses of potential divider circuits
Topic C: Wave Behaviour
C.1 Simple Harmonic Motion
Explain the two conditions necessary for an object to oscillate with Simple Harmonic Motion
Recognise and use the defining equation for SHM, understanding the significance of the negative sign in a = -ω²x
Define time period T, frequency f, angular frequency ω, amplitude A, equilibrium position and displacement in terms of a particle in SHM
Calculate time period, T for one complete oscillation for (1) a particle undergoing SHM, (2) a mass-spring system and (3) a simple pendulum
Describe the energy changes during one oscillation of an object undergoing SHM
Sketch and interpret graphs of examples of simple harmonic motion (including displacement-time, velocity-time, acceleration-time and acceleration-displacement graphs)
C.1 Simple Harmonic Motion (HL)
Understand and explain how the phase angle φ is used to describe the state of a particle undergoing simple harmonic motion.
Calculate properties of an SHM oscillator
Describe the interchange of kinetic and potential energy during SHM, and solve problems using both graphical and algebraic methods
C.2 Wave Model
Explain the motion of particles for both transverse and longitudinal waves
Sketch and interpret displacement-distance graphs and displacement-time graphs for transverse and longitudinal waves
Define wavelength, frequency, time period, wave speed and amplitude
Be able to derive v=fλ and solve problems using this equation
Compare the nature of sound waves and electromagnetic waves
C.3 Wave Phenomena
Explain that waves travelling in two and three dimensions can be described through the concepts of wavefronts and rays
Define wave behaviour at boundaries in terms of reflection, refraction and transmission
Describe and sketch wave diffraction around a body and through an aperture
Sketch incident, reflected and transmitted wavefronts/rays between media (i.e. refraction)
Solve problems involving Snell's law, critical angle and total internal reflection
Be able to calculate the superposition of two waves / wave pulses
Describe the conditions necessary for double source interference
State the conditions necessary for constructive and destructive interference as given by path length difference
Understand the significance of Thomas Young's double slit experiment in the proof of light as a wave. Select and use s=λD/d for double slit experiments
C.3 Wave Phenomena (HL)
Single Slit Diffraction at normal incidence through a rectangular slit:
Describe the effect of changing the slit width
Determine the position of the first interference medium
Describe diffraction pattern produced from monochromatic light
Describe the interference pattern produced by a double slit on a screen, including the modulation by the single slit diffraction effect
Sketch and interpret intensity graphs of double slit interference patterns
Distinguish between the width of the slits and the separation of the slits in accounting for their effects on intensity graphs
Recognise that multiple slits and diffraction gratings can create interference patterns by considering path difference (for white light and a range of monochromatic light). Select and use nλ=d sinθ for diffraction grating problems
C.4 Standing Waves and Resonance
Describe the conditions necessary for the formation of standing waves
Draw diagrams and identify nodes and antinodes, relative amplitude and phase difference of points along a standing wave
Describe the formation of standing waves in terms of superposition (standing wave patterns in strings and pipes). Boundary conditions for:
Strings: two fixed boundaries, one fixed and one free boundary, and two free boundaries
Pipes: two closed ends, one closed and one open end, and two open ends
Solve problems involving the frequency of a harmonic, length of the standing wave and the speed of the wave
Explain and give examples of useful and destructive resonance including natural frequency and amplitude of oscillation based on driving frequency
Graphically describe the variation of the amplitude of vibration with driving frequency of an object close to its natural frequency of vibration
Describe the effects of light, critical and heavy damping on the system
C.5 Doppler Effect
Sketch and interpret the Doppler effect (for sound and electromagnetic waves) when there is relative motion between source and observer
Describe situations where the Doppler effect can be used (i.e. radars, red-shift of receding galaxies, moving objects emitting sound, ultrasounds reflected from blood cells, radars, etc.)
Recognise that electromagnetic waves (i.e. red-shift of galaxies) requires that the approximation equation should be used:
Δf / f = Δλ / λ ≈ v / c
Explain how shifts in spectral lines provide information about the motion of bodies like stars and galaxies in space.
C.5 Doppler Effect (HL)
Solve problems involving the change in frequency or wavelength observed due to the Doppler effect to determine the velocity of the source/observer
Topic D: Fields
D.1 Gravitational Fields
State Kepler's three laws of motion
Solve problems using Newton's Law of Gravitation between two spherical masses, where the masses are assumed to have uniform density and mass is concentrated at the centre
Recognise that when astronomical objects are in orbit, the gravitational force is equal to the centripetal force
Recall the definition for gravitational field strength
Determine the resultant gravitational field strength due to two bodies (restricted to points along the straight line adjoining the bodies)
Sketch the gravitational field lines for:
Radial field surrounding point or spherical masses
Uniform field close to the surface of massive celestial bodies and planetary bodies
D.1 Gravitational Fields (HL)
Define gravitational potential energy and determine the potential energy of a point mass
Recognise gravitational potential, Vₚ, as a scalar and defined as the work per unit mass in bringing a small test mass from infinity to point P (units Jkg⁻¹)
Recognise the magnitude of the gravitational field as the rate of change of potential with distance
Draw equipotential lines on gravitational fields and explain that moving between equipotential lines requires work to be done on the point mass
Define escape speed and solve problems involving the speed required for an object to escape the gravitational field of a planet
Describe the qualitative effect of a small viscous drag force due to the atmosphere on the height and speed of an orbiting body
D.2 Electric and Magnetic Fields
Know that there are positive and negative charges and predict the direction of forces between them
Solve problems using Coulomb's Law
State the law of conservation of electric charge
Describe Millikan’s experiment as evidence for quantisation of charge
Describe how electric charge can be transferred between bodies using friction, electrostatic induction and by contact, including the role of grounding (earthing)
Calculate the electric field strength of a uniform electric field
Sketch the electrostatic field lines for:
Radial field surrounding point or spherical charges
Inside and outside a spherical conducting body
Between two like or opposite charges
Uniform field lines between charged parallel plates (with edge effect)
Recognise that a higher field line density represents a larger electric field strength
Sketch magnetic field patterns around a bar magnet, a current-carrying wire, a current-carrying singular coil and an air core solenoid
Determine the direction of magnetic field around a long, straight current-carrying wire
D.2 Electric and Magnetic Fields (HL)
Define electric potential energy and determine the potential energy for a system of two charged bodies
Recognise electric potential as a scalar and defined as the work per unit charge in bringing a small test charge from infinity to point P
Recognise the magnitude of the electric field strength as the rate of change of potential with distance
Draw equipotential surfaces and explain that moving between equipotential lines requires work to be done on the point charge
D.3 Motion in Electromagnetic Fields
Describe the motion of a charged particle in:
A uniform electric field
A uniform magnetic field
Perpendicularly orientated uniform electric and magnetic fields
Calculate the magnitude and direction of the force on a charge moving in a magnetic field
State that the magnetic force provides the centripetal force for a charged particle moving in a magnetic field
Calculate the charge-to-mass ratio for a charged particle by investigating its path in a uniform magnetic field
Calculate the magnitude and direction of the force on a current-carrying conductor in a magnetic field
Calculate the magnitude and direction of the force per unit length between current-carrying parallel wires
D.4 Induction (HL)
Define Magnetic Flux
Recall and use Faraday's Law
Calculate the emf induced by a straight conductor moving perpendicularly to a uniform magnetic field
Explain Lenz's Law through conservation of energy
Explain how an emf is induced in the following situations:
Fixed coils in a changing magnetic field
AC generators
Explain the operation of a basic AC generator, including the effect of the generator frequency
Topic E: Nuclear and Quantum Physics
E.1 Structure of the Atom
Describe Rutherford's scattering experiment, including the three main observations and conclusions of the structure of the atom
Understand that the absorption and emission spectra for each element is unique
Explain how spectral lines are evidence for the existence of discrete energy levels
Describe how emission and absorption spectra are produced
Calculate the frequency (or wavelength) of released or absorbed photons using the energy difference between energy levels in an atom
E.1 Structure of the Atom (HL)
Calculate the radius of a nucleus and recognise that nuclear densities are approximately the same for all nuclei
Explain how the results of Rutherford's experiment change when higher energy alpha particles are used
Use energy conservation considerations to calculate the distance of closest approach in head-on scattering experiments to find the approximate value for the density of a nucleus
Describe the discrete energy levels in the Bohr model for the hydrogen atom and understand the terms of the quantisation of angular momentum
E.2 Quantum Physics (HL)
Describe a photon as a quanta of energy and momentum
Discuss the photoelectric effect and explain why the classical theory of light means a wave cannot be explained by the photoelectric effect. Define the work function and threshold frequency.
Solve problems about the photoelectric effect
Interpret the following graphs relating to the photoelectric effect:
Kinetic energy (y-axis) against frequency (x-axis)
Current (y-axis) against voltage (x-axis)
Stopping voltage (y-axis) against 1/λ (x-axis)
Recognise that matter can have wave-like properties (wave-particle duality)
Describe the experiment where electrons can be accelerated and diffracted through a thin graphite film, thus proving the wave nature of electrons
Calculate the de Broglie wavelength for particles
Explain how the Compton scattering of photons off electrons with increased wavelength is additional evidence of the particle nature of light
Calculate the shift in photon wavelength after scattering off an electron
E.3 Radioactive Decay
Define an isotope
Solve problems involving mass defect, binding energy and the atomic mass unit (memorise 1u = 931MeV)
Define the mass-energy equivalence as given by E = mc² in nuclear reactions
Recall the definition for Binding Energy
Sketch and understand the general shape of the graph for average binding energy per nucleon against nucleon number
Calculate the frequency (or wavelength) of released or absorbed photons using the energy difference between energy levels in an atom
Define strong nuclear force
Describe the properties of alpha, beta and gamma radiation, including changes of state of nucleus, penetration, ionizing ability and real-life contexts
Complete decay equations for radioactive decay
Recognise that there are two types of beta decay (β⁻ and β⁺) and explain the existence of neutrinos and anti-neutrinos
Define activity, count rate and half-life in radioactive decay
Determine the half-life of a radioactive nuclide using a decay curve or simple integral calculations, including the effect of background radiation
E.3 Radioactive Decay (HL)
Describe evidence for the strong nuclear force
Understand the role of the ratio of neutrons to protons for the stability of nuclides
State that the spectrum of alpha and gamma radiations provides evidence for discrete nuclear energy levels
State the continuous spectrum of beta decay as evidence for the neutrino
Define the decay constant
Explain that the decay constant approximates only in the limit of sufficiently small λt
Calculate the number of undecayed nuclei, activity and half-lives in radioactive decay for arbitrary time intervals
E.4 Fission
Describe how energy is released in spontaneous and neutron-induced fission
Calculate how much energy is released in a nuclear fission reaction
Describe the role of chain reactions in nuclear fission reactions
Explain the role of control rods, moderators, heat exchangers and shielding in a nuclear power plant
Describe the properties of the products of nuclear fission and their management, including the impact of long-term storage
E.5 Fusion and Stars
Explain how a star maintains equilibrium through the balance between radiation pressure and gravitational forces
Discuss nuclear fusion as the energy source of stars, outlining the necessary conditions for fusion and key reactions occurring in main-sequence stars
Compute the energy output from fusion reactions
Draw and analyze Hertzsprung-Russell (HR) diagrams, identifying main sequence stars, red giants, supergiants, white dwarfs, the instability strip, and constant-radius lines
Interpret HR diagrams with luminosity on the vertical axis and temperature on the horizontal axis
Convert distances between astronomical units (AU), light-years (ly), and parsecs (pc)
Apply the method of stellar parallax to measure distances to stars
Determine a star’s surface temperature using its spectrum, employing intensity-wavelength graphs and Wien’s Displacement Law
Analyze a star’s absorption spectrum to infer its chemical composition
Use luminosity and surface temperature data to calculate the radius of a star