IB Physics Syllabus 2025
Simplifying the 2025 IB Physics Syllabus for You
If it's not in the syllabus, it's not in the IB Physics exam
In this article, I'll break down the new 2025 IB Physics syllabus into easytounderstand sections. You’ll find a downloadable PDF of the syllabus, simplified into a checklist of learning objectives, along with helpful tips on how to use the syllabus effectively.
The new IB Physics guide covers fewer topics than the old specification. It focuses on the most important ideas in Physics, which will help you understand and connect different types of knowledge better. You'll keep learning new things, build on what you know, and fix any mistakes along the way.
Teaching Order
The syllabus now includes main ideas like energy, forces, and particles in a flexible plan. This means your teacher can create the best learning path for you over the two years.
This syllabus is designed for teachers to teach the course in any order; however, most teachers will start at the very beginning and work linearly through it.
Teaching Hours
Your school should allocate 150 hours of teaching for the SL course and 240 hours for the HL IB Physics course.
The IB have given an indication of how many hours should be allocated to teach each theme:
This allocation of teaching hours gives a clear indication of how important each topic is for the final exams.
I've done detailed analysis on the breakdown of teaching hours and have created a priority list of topics for IB Physics exam revision. Head to my other article, "How To Study IB Physics" for more information on how to be strategic in your study and use this information to your advantage.
Comprehensive Learning Objectives for IB Physics
Below, you'll find a comprehensive list of everything you need to know for the new IB Physics examinations syllabus, which starts teaching in September 2023.
I've helped thousands of IB Physics students to get a 7, and here’s how you can too! With GradePod’s expertly crafted resources, you’ll have everything you need to succeed.
Every, single learning objective below is taught inside TrIBe Physics; using key concept videos, practice exam questions, screencast solutions and direct access to Chief Physics Innovator, Sally Weatherly.
Honestly.... the TrIBe Physics program is awesome! You get personalised support and guidance from me (with direct access), meaning you can significantly improve your understanding of Physics concepts and excel in your exams. Don't forget there is a 💯 moneyback grade guarantee on the lifetime plan  meaning there is no risk for you 💪😊 
A.1 Kinematics
 Define displacement, velocity and acceleration
 Explain the difference between distance and displacement
 Calculate instantaneous and average values of velocity, speed, and acceleration
 Recognise situations where acceleration is uniform and nonuniform
 Understand that the equations of motion are only valid for uniformly accelerated motion
 Solve problems using the equations of motion
 Define a projectile and resolve into vertical and horizontal components
 Solve projectile motion problems for horizontal, oblique, and below horizontal projections (assuming negligible or absent air resistance, and close to the earth's surface with an acceleration of 'g')
 Describe the effects of air resistance on the trajectory path, time of flight, velocity, acceleration, and terminal speed of a projectile.
A.2 Forces and Momentum
 State Newton’s three laws of motion
 Solve translational equilibrium problems using Newton’s 1st Law
 Identify force pairs using Newton’s 3rd Law
 Describe forces as interactions between bodies
 Draw freebody diagrams and analyse them to find the resultant force on a system in one and two dimensions only
 Understand the nature and use the following contact forces:
normal, frictional, elastic, viscous drag, buoyancy  Understand the nature and use of the following field forces: gravitational, electric, magnetic
 Define linear momentum and understand that it remains constant unless the system is acted upon by a resultant external force
 Define Impulse as a resultant external force applied to a system and recall that impulse equals the change in momentum of the system
 Derive Newton’s 2nd Law from the definition of net force as the rate of change of a momentum of an object, when mass is constant
 Solve problems using momentum and impulse for collisions and explosion (one dimensional for SL and two dimensional for HL)
 Understand the scenarios of elastic/inelastic collisions and explosions
 State that bodies undergoing circular motion travel at a constant speed but still experience acceleration directed radially towards the centre of the circle
 Draw a vector diagram to illustrate that the acceleration of a particle moving with constant speed in a circle is directed towards the centre of the circle.
 Recognise the direction of velocity, acceleration and force vectors for an object in circular motion.
 Understand and solve problems involving centripetal force, centripetal acceleration, period, frequency, angular displacement, linear speed and angular velocity.
A.3 Work, Energy and Power

State the principle of the conservation of energy

Recall that work done by a force is equal to the energy transferred in the system

Sketch and analyse energy transfers on Sankey diagrams

Determine work done (using W = Fscosθ) including cases where a resistive force acts and where force and distance are not parallel.

Recall and solve problems using fact that the mechanical energy of a system is the sum of kinetic energy, gravitational potential energy and elastic potential energy, in the absence of frictional forces.

Solve problems using the appropriate relationships for work done and energy transferred in systems where mechanical energy is conserved.

Define Power as the rate of work done, or rate of energy transfer.
Solve problems involving power. 
Define efficiency in terms of energy transfer or power. Solve problems involving efficiency.

Define and solve problems of the energy density of a fuel source
A.4 Rigid Body Mechanics (HL ONLY)

Describe the torque τ of a force about an axis

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 ⍵ 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. ∆L=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 ONLY)

Define a reference frame and 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'=xvt 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.
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 StefanBoltzmann 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 manmade 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 laws 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 Only)

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
 Solving 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 nonohmic 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, lightdependent resistors (LDR) and potentiometers
 Describe practical uses of potential dividers circuits
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 = ω(^2)x

Define time period T, frequency f, angular frequency ⍵, 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 massspring 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 displacementtime, velocitytime, accelerationtime and accelerationdisplacement graphs)
Simple Harmonic Motion (HL Only)
 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 displacementdistance 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
Wave Phenomena (HL ONLY)
 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=dsinθ for diffraction grating problems
C.4 Standing Waves and Resonance

Describe the conditions necessary for the formation of standing wave

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 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, redshift of receding galaxies, moving objects emitting sound, ultrasounds reflected from blood cells, radars, etc.)

Recognise that electromagnetic waves (i.e. redshift of galaxies) requires that the approximation equation should be used

Explain how shifts in spectral lines provide information about the motion of bodies like stars and galaxies in space.
Doppler Effect (HL ONLY)
 Solve problems involving the change in frequency or wavelength observed due to the Doppler effect to determine the velocity of the source/observer
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:
i) radial field surrounding point or spherical masses and
ii)uniform field close to the surface of massive celestial bodies and planetary bodiesGravitational Fields (HL ONLY)
 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
 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:
i) radial field surrounding point or spherical charges,
ii) inside and outside a spherical conducting body,
iii) between two like or opposite charges and
iv) 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 currentcarrying wire, a currentcarrying singular coil and an air core solenoid

Determine the direction of magnetic field around a long, straight currentcarrying wire
Electric and Magnetic Fields (HL ONLY)
 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

Know that there are Describe the motion of a charged particle in
(1) a uniform electric field
(2) uniform magnetic field and
(3) perpendicularly orientated uniform electric and magnetic fields 
Calculate the magnitude and direction of the force on a charge moving in a magnetic field

State the magnetic force provides the centripetal force for a charged particle moving in a magnetic field

Calculate the chargetomass 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 currentcarrying parallel wires
D.4 Induction (HL Only)

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: i) fixed coils in a changing magnetic field, and ii) ac generators

Explain the operation of a basic ac generator, including the effect of the generator frequency
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
Structure of the Atom (HL ONLY)
 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 headon 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 Only)

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 (yaxis) against frequency (xaxis)
current (yaxis) against voltage (xaxis)
stopping voltage (yaxis) against 1/λ (xaxis) 
Recognise that matter can have wavelike properties (waveparticle duality)

Describe the experiment where electrons can be accelerated and diffracted through a thing 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) using

Define the massenergy equivalence as given by E = mc^2 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 reallife 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 antineutrinos

Define activity, count rate and halflife in radioactive decay

Determine the halflife of a radioactive nuclide using a decay curve or simple integral calculations, including the effect of background radiation
Radioactive Decay (HL ONLY)
 Describe evidence for the strong nuclear force
 Understand the role of that ration 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 halflives in radioactive decay for arbitrary time intervals
E.4 Fission

Describe how energy is released in spontaneous and neutroninduced 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 longterm storage
E.5 Fusion and Stars

Describe the equilibrium between radiation pressure and gravitation in stars  how the star then achieves stellar equilibrium

Describe fusion as the source of energy in stars, the conditions required for fusion to occur and the basic fusion reactions present in stars on the mainsequence

Calculate the energy released in fusion reactions

Sketch and interpret HR diagrams, including the location of main sequence stars, red giants, super giants, white dwarfs, the instability strip and lines of constant radius

HR diagrams will be labelled with luminosity on the vertical axis and temperature

Convert between astronomical units (AU), light years (ly) and parsecs (pc)

Use stellar parallax as a method to determine the distance to celestial bodies

Explain how surface temperature may be obtained from a star’s spectrum, using intensitywavelength graphs and/or Wien’s Displacement Law

Explain how the chemical composition of a star may be determined from the star’s spectrum, using the absorption spectrum of light received from the star

Calculate stellar radii using luminosity and surface temperature
Practical Work
You can expect 20 hours of practical work in the SL course and 40 hours in the HL course.
There are no EXACT rules for which practicals you'll complete; however, the IB Physics syllabus does set out some expectations for:
 Experimental Skills
 Technology
The practicals that your teacher designs should meet the requirements of these skills
Experimental Techniques
You must know which apparatus to use to measure the following quantities:
 Mass
 Time
 Length
 Volume
 Temperature
 Force
 Electric current
 Electric potential difference
 Angle
 Sound and light intensity
You'll also need to know possible systematic and random errors that might arise using this apparatus.
The practicals that your teacher designs should help you understand the appropriate level of precision for these variables too. For example, you’d want to measure the length of a wire to the nearest millimetre, any less precise would not be appropriate.
Technology
The experiments you carry out in class should allow you to use modern technology to both collect and analyse the data.
You'll need to be able to use the following technology to collect data:
 Datalogging sensors and/or smartphone apps (e.g. measuring light intensity using a smartphone sensor)
 Spreadsheets and databases to extract data
 Generate data from models and simulations.
 Carry out image analysis and video analysis of motion (e.g. use a slow motion camera to analyse the motion of a toy parachute in freefall)
You'll need to use the following technology to analyse the data:
 Use spreadsheets to manipulate data.
 Represent data in a graphical form.
 Use computer modelling.
It’s your teacher’s responsibility to include this into your lessons over the two year course at school. You do not need to prepare this for exams.
Practical work is a key part of learning physics. You'll be doing experiments in the classroom, lab, or even outdoors. These experiments are not just about following instructions—they're about exploring topics, understanding phenomena, and diving into real questions you might be curious about.
Your school's experimental program is designed to give you a full experience of the physics course. You'll develop scientific skills and learn how to use different tools and techniques safely and effectively. You'll get to do a variety of investigations, from handson lab and fieldwork experiments to working with databases, simulations, and models.
What are the main themes covered in the IB Physics syllabus?
How many teaching hours are allocated for the IB Physics syllabus?
How many hours of practical work are required in the IB Physics syllabus?
Are there specific practical experiments I need to complete for the IB Physics syllabus?
Can teachers choose the order in which they teach the IB Physics syllabus?
Where can I find additional resources to help with my studies for IB Physics?
Extra Help With IB Physics
If you need help with any of IB Physics, consider joining TrIBe Physics. It has everything you need to get that 7 in IB Physics.