Physics
G3N tutors you through the full NERDC Physics syllabus offline — from Theme 1: Measurement and Motion, Theme 2: Forces and Momentum, Theme 3: Properties of Matter and more — with adaptive lessons, instant quizzes, flashcards and exam-ready summaries.
Syllabus
What you’ll cover in Physics.
The complete topic outline G3N teaches, mapped to the NERDC curriculum.
SSS 1
5 topicsTheme 1: Measurement and Motion
- Physical Quantities and Units
- Define physics as the scientific study of matter, energy, motion, and forces in the universe
- Identify the seven SI base units: length (metre, m), mass (kilogram, kg), time (second, s), electric current (ampere, A), temperature (kelvin, K), amount of substance (mole, mol), luminous intensity (candela, cd)
- Derive SI derived units: area (m²), volume (m³), velocity (m/s), acceleration (m/s²), force (N = kg·m/s²), pressure (Pa = N/m²), energy (J = N·m)
- Apply dimensional analysis: express quantities in different units using dimensional symbols [M], [L], [T]
- Recognize and correct systematic and random measurement errors
- Use appropriate significant figures and express measurements with uncertainty
- Convert between units using conversion factors: km/h to m/s, cm² to m², g/cm³ to kg/m³
- Understand accuracy (closeness to true value) vs. precision (consistency of measurements)
- Mechanics: Kinematics
- Define scalar quantities (magnitude only): distance, speed, time; vector quantities (magnitude and direction): displacement, velocity, acceleration
- Represent vectors graphically as arrows: length represents magnitude, direction indicates direction
- Calculate displacement: change in position with direction (different from distance traveled)
- Calculate velocity: rate of change of displacement; distinguish from speed (distance/time)
- Calculate acceleration: rate of change of velocity; use a = (v - u)/t for constant acceleration
- Apply kinematic equations of motion: v = u + at, s = ut + (1/2)at², v² = u² + 2as
- Plot and interpret position-time graphs: gradient = velocity, straight line = constant velocity
- Plot and interpret velocity-time graphs: gradient = acceleration, area under curve = displacement
Theme 2: Forces and Momentum
- Newton's Laws of Motion
- State Newton's First Law: object at rest stays at rest, object in motion stays in motion unless acted upon by unbalanced force; define inertia as resistance to acceleration
- State Newton's Second Law: F = ma; force causes acceleration proportional to force and inversely to mass
- Apply F = ma to calculate forces and accelerations in real scenarios
- State Newton's Third Law: for every action, there is an equal and opposite reaction
- Identify action-reaction pairs: understand that they act on different objects
- Apply Newton's laws to systems with multiple forces: resolve forces into components, find net force
- Analyze friction: static friction (prevents motion), kinetic friction (opposes motion); f = μN
- Apply Newton's laws to inclined planes: resolve weight into components parallel and perpendicular to surface
- Work, Energy, and Power
- Define work as force applied over distance in direction of force: W = F·s·cosθ (scalar product)
- Distinguish between positive work (force aids motion), negative work (force opposes motion), zero work (force perpendicular)
- Define kinetic energy: KE = (1/2)mv²; energy of motion
- Define potential energy: gravitational PE = mgh; elastic PE = (1/2)kx² for springs
- Apply work-energy theorem: net work equals change in kinetic energy (W = ΔKE)
- Apply conservation of mechanical energy: total energy = KE + PE = constant (in absence of friction)
- Analyze energy transformations: kinetic ↔ potential, with/without energy loss
- Define power as work done per unit time: P = W/t (watts); relate to rate of energy transfer
- Momentum and Collisions
- Define momentum: p = mv (mass × velocity); vector quantity with direction of velocity
- Define impulse: I = F·Δt or I = Δp (change in momentum); force applied over time interval
- Apply impulse-momentum theorem: impulse equals change in momentum (F·Δt = Δp)
- Apply conservation of momentum: total momentum before collision = total momentum after (in isolated system)
- Analyze elastic collisions: kinetic energy is conserved; objects separate after collision
- Analyze inelastic collisions: kinetic energy is lost; objects may stick together
- Apply conservation of momentum to two-body collisions: calculate velocities after collision
- Understand explosion and recoil: momentum conservation in systems that separate
Theme 3: Properties of Matter
- States of Matter
- Describe solid state: particles in fixed, regular arrangement; strong intermolecular forces; fixed shape and volume
- Describe liquid state: particles in random arrangement but in contact; moderate forces; fixed volume, shape of container
- Describe gaseous state: particles far apart with high kinetic energy; weak forces; expands to fill container
- Understand particle model of matter: all matter made of particles with spaces between
- Relate particle motion to temperature: higher temperature = faster particle motion
- Apply kinetic model: pressure from particles colliding with container walls; P = (1/3)ρc² (rms speed relation)
- Understand phase changes: melting (solid→liquid), evaporation (liquid→gas), sublimation (solid→gas), and reverse processes
- Identify latent heat: energy required for phase changes without temperature change
- Fluid Mechanics
- Define pressure: force per unit area (P = F/A); SI unit pascal (Pa = N/m²)
- Calculate pressure in fluids: pressure = ρgh for liquids (depends on depth, not shape)
- Apply Pascal's principle: pressure applied to fluid transmitted equally in all directions
- Understand hydraulic systems: use pressure transmission to amplify force (F₁/A₁ = F₂/A₂)
- Define and calculate atmospheric pressure: approximately 101,325 Pa at sea level
- Apply Archimedes' principle: upthrust equals weight of displaced fluid
- Calculate buoyancy: F = ρ_fluid·g·V_submerged
- Determine if objects float: compare object density to fluid density; objects float if density less than fluid
Theme 4: Heat and Thermodynamics
- Thermal Properties
- Distinguish between temperature (average kinetic energy of particles) and heat (thermal energy transfer)
- Identify temperature scales: Celsius (0° = water freezes, 100° = boils), Kelvin (T(K) = T(°C) + 273.15)
- Define thermal energy: total kinetic energy of all particles in object
- Calculate heat energy: Q = m·c·ΔT where c is specific heat capacity
- Understand specific heat capacity: energy to raise 1kg by 1°C; varies by material
- Identify heat transfer mechanisms: conduction (contact), convection (fluid movement), radiation (electromagnetic waves)
- Analyze thermal conduction: rate depends on material, temperature difference, thickness; Q/t = kA(ΔT)/d
- Understand thermal expansion: volume increases as temperature increases; V = V₀(1 + β·ΔT)
- Thermodynamics
- State the First Law of Thermodynamics: ΔU = Q - W (change in internal energy = heat added - work done by system)
- Define internal energy: total energy of particles in system (kinetic + potential from intermolecular forces)
- Interpret First Law: energy cannot be created/destroyed; account for all energy transfers
- Calculate work done: W = P·ΔV for constant pressure processes
- Identify isobaric processes (constant pressure): work done by gas, heat absorbed, temperature change
- Identify isochoric (constant volume) processes: no work done, all heat goes to internal energy
- Identify isothermal processes (constant temperature): internal energy unchanged, work = heat
- State the Second Law of Thermodynamics: entropy increases in isolated systems; heat flows from hot to cold
Theme 5: Waves and Sound
- Wave Motion
- Define transverse waves: particle oscillation perpendicular to wave direction (e.g., light, water ripples)
- Define longitudinal waves: particle oscillation parallel to wave direction (e.g., sound, compressions)
- Identify wave characteristics: wavelength λ (distance between successive crests), frequency f (oscillations per second)
- Define wave speed: v = f·λ (frequency × wavelength)
- Understand amplitude: maximum displacement from equilibrium; relates to wave intensity
- Apply wave equation: y = A·sin(2π(x/λ - t/T)) or v = f·λ
- Analyze wave superposition: when waves overlap, amplitudes add; constructive interference (amplitudes same direction) vs. destructive (opposite)
- Identify standing waves: waves reflected back and forth creating nodes (no motion) and antinodes (maximum motion)
- Sound Waves
- Identify sound as longitudinal mechanical waves: compressions and rarefactions of air/medium
- Define frequency and pitch: higher frequency = higher pitch; human hearing range ~20 Hz to 20,000 Hz
- Understand speed of sound: ~343 m/s in air at 20°C; varies with medium and temperature
- Calculate speed using v = f·λ for sound waves
- Define intensity: power per unit area; measured in W/m²; relates to perceived loudness
- Understand sound level: decibel scale (dB) is logarithmic; each 10 dB increase is 10× intensity
- Apply Doppler effect: observed frequency changes when source moves relative to observer; f' = f(v ± v_observer)/(v ∓ v_source)
- Understand resonance: object vibrates with maximum amplitude at its natural frequency
SSS 2
4 topicsTheme 1: Vibrations and Oscillations
- Simple Harmonic Motion
- Define simple harmonic motion (SHM): motion where acceleration is proportional to displacement in opposite direction (a = -ω²x)
- Identify conditions for SHM: restoring force proportional to displacement (F = -kx)
- Calculate angular frequency: ω = 2πf; period T = 1/f = 2π/ω
- Analyze mass-spring system: period T = 2π√(m/k); independent of amplitude
- Analyze simple pendulum: period T = 2π√(L/g) where L is length, g is gravitational acceleration
- Apply equations of SHM: x = A·cos(ωt + φ), v = -Aω·sin(ωt + φ), a = -Aω²·cos(ωt + φ)
- Understand energy in SHM: total energy E = (1/2)kA²; transforms between kinetic and potential
- Analyze damped oscillations: amplitude decreases with time due to energy loss (friction, air resistance)
Theme 2: Electricity and Magnetism
- Electrostatics
- Define electric charge: fundamental property of matter; electrons (-e), protons (+e); 1 e = 1.6 × 10⁻¹⁹ C
- Understand Coulomb's law: F = k·q₁·q₂/r² (force between charges); k = 8.99 × 10⁹ N·m²/C²
- Define electric field: force per unit charge; E = F/q (N/C); shows effect of charges on surroundings
- Calculate field strength: E = kQ/r² for point charge; E = σ/ε₀ for uniform field
- Visualize electric field: field lines point from positive to negative charges; density indicates field strength
- Define electric potential: energy per unit charge; V = W/q (volts); V = kQ/r for point charge
- Understand potential difference: voltage between two points; ΔV = V_B - V_A
- Relate field and potential: E = -dV/dx; field points from high to low potential
- Electric Current
- Define electric current: flow of charge; I = Q/t (amperes); direction is flow of positive charge
- Understand drift velocity: slow movement of electrons; related to current by I = nAe·v_d
- Define resistance: opposition to current flow; R = V/I (ohms); Ohm's law
- Understand resistivity: R = ρL/A; property of material; varies with temperature
- Calculate total resistance: series R_total = R₁ + R₂ + ... (current same); parallel 1/R_total = 1/R₁ + 1/R₂ + ...
- Define electromotive force (EMF): energy per unit charge provided by source; ε = W/Q
- Understand internal resistance: resistivity of battery/source; terminal voltage = ε - Ir
- Apply Kirchhoff's voltage law: sum of potentials around circuit = 0; track voltage changes
- Magnetism
- Identify magnetic poles: north (N) and south (S); opposite poles attract, same poles repel
- Understand magnetic field: force region around magnets; shown by field lines (N to S pole outside magnet)
- Define magnetic field strength: B (tesla, T); measure of magnetic effect
- Understand magnetic force on current: F = I·L·B·sinθ where L is conductor length, θ is angle to field
- Apply force on moving charge: F = q·v·B·sinθ; basis for motion in magnetic fields
- Calculate magnetic field from straight wire: B = (μ₀I)/(2πr); μ₀ = 4π × 10⁻⁷ T·m/A
- Analyze magnetic force in circuits: force on conductors in magnetic fields; used in motors
- Understand electromagnetic induction: changing magnetic flux induces EMF; ε = -N·dΦ/dt (Faraday's law)
Theme 3: Light and Optics
- Geometric Optics
- Understand reflection: incident angle = reflected angle (from normal); mirror equation 1/f = 1/u + 1/v
- Analyze plane mirrors: image virtual, upright, same size; magnification m = -v/u = 1
- Analyze curved mirrors: concave (converging) and convex (diverging); use 1/f = 1/u + 1/v
- Understand refraction: light bends when entering different medium; Snell's law n₁sinθ₁ = n₂sinθ₂
- Define refractive index: n = c/v (speed of light in vacuum / speed in medium)
- Analyze lens types: convex/converging (positive f) and concave/diverging (negative f)
- Apply lens equation: 1/f = 1/u + 1/v; valid for thin lenses
- Calculate magnification: m = -v/u (negative = inverted); use to determine image orientation
- Wave Properties of Light
- Understand diffraction: light bends around obstacles; more pronounced for longer wavelengths
- Analyze single-slit diffraction: creates central maximum and side minima; minima at x·sinθ = n·λ
- Analyze double-slit interference: creates alternating maxima (bright) and minima (dark); maxima at d·sinθ = n·λ
- Understand interference pattern spacing: Δy = λL/d (wavelength × distance / slit separation)
- Analyze diffraction grating: many slits create sharp maxima; used to measure wavelength and resolve lines
- Understand polarization: light vibrations in one plane; achieved by filters, reflection, or birefringent materials
- Apply Malus's law: I = I₀·cos²θ (intensity through polarizers at angle θ)
- Understand electromagnetic spectrum: visible light (λ ≈ 400-700 nm) part of spectrum from radio to gamma rays
Theme 4: Modern Physics Introduction
- Atomic Physics
- Understand photoelectric effect: electrons emitted when light hits metal; Einstein's equation E = hf = Φ + KE_max
- Define work function Φ: minimum energy to remove electron; explains threshold frequency
- Analyze photoelectric effect: photon energy (hf) must exceed work function; KE increases with frequency
- Understand Bohr's model: electrons in discrete orbits; energy E_n = -13.6/n² eV for hydrogen
- Apply energy levels: transitions between levels emit/absorb photons; ΔE = hf
- Identify emission spectra: specific wavelengths emitted; due to electron transitions
- Identify absorption spectra: dark lines in continuous spectrum; wavelengths absorbed match emission
- Understand quantum numbers: n (principal), l (orbital), m_l (magnetic), m_s (spin)
- Nuclear Physics
- Understand nucleus: protons (Z) and neutrons (N = A - Z) bound together; A = mass number
- Define nuclear binding energy: energy holding nucleus together; related to mass defect by E = Δm·c²
- Understand radioactivity: unstable nuclei decay to reach stability
- Identify alpha decay (⁴₂He): nucleus loses helium nucleus; A decreases by 4, Z by 2
- Identify beta decay (β⁻): neutron → proton + electron + antineutrino; N decreases by 1, Z increases by 1
- Identify gamma decay (γ): nucleus loses energy as high-energy photons; A and Z unchanged
- Understand half-life: time for half of sample to decay; N(t) = N₀·(1/2)^(t/t₁/₂)
- Analyze nuclear equations: ensure mass number and atomic number conserved
SSS 3
4 topicsTheme 1: Advanced Relativity
- Special Relativity
- Understand relativity of motion: measurements depend on observer's reference frame
- Apply Einstein's postulates: laws of physics same in all inertial frames; speed of light constant
- Understand time dilation: moving clock runs slow; Δt = Δt₀/√(1-v²/c²) where Δt₀ is proper time
- Apply length contraction: moving objects shortened in direction of motion; L = L₀√(1-v²/c²)
- Understand mass-energy equivalence: E = mc² converts between mass and energy
- Apply relativistic energy: E² = (pc)² + (mc²)² relates energy, momentum, mass
- Understand particle creation: pair production (photon → particle + antiparticle) and annihilation
- Analyze relativistic motion: momentum p = γmv; force still F = dp/dt
Theme 2: Quantum Mechanics
- Quantum Theory
- Understand Planck's quantum hypothesis: energy of photon E = hf = hc/λ; relates to frequency
- Define wave-particle duality: all matter has wave properties; wavelength λ = h/p (de Broglie relation)
- Understand uncertainty principle: Δx·Δp ≥ ℏ/2; cannot know position and momentum simultaneously
- Interpret Schrödinger equation: wave function ψ describes quantum state; |ψ|² = probability density
- Understand quantum tunneling: particles can pass through potential barriers; probability non-zero inside barrier
- Apply to practical systems: scanning tunneling microscope, radioactive decay, semiconductor devices
- Understand quantum superposition: particles can be in multiple states simultaneously until measured
- Understand measurement collapse: measurement forces quantum system into definite state
Theme 3: Nuclear and Particle Physics
- Advanced Nuclear Physics
- Calculate binding energy: B.E. = Δm·c² where Δm = Zm_p + Nm_n - M_nucleus
- Understand binding energy per nucleon: indicates nuclear stability; peaks at iron-56
- Analyze fission reactions: heavy nucleus splits into lighter nuclei; releases energy
- Apply chain reaction: one fission triggers multiple fissions; controlled (power plants) or uncontrolled (weapons)
- Analyze fusion reactions: light nuclei combine; releases more energy per nucleon than fission
- Understand deuterium and tritium: isotopes used in fusion; hydrogen bomb and fusion reactors
- Detect particles: Geiger counter, cloud chamber, scintillation detector measure radiation
- Understand particle accelerators: accelerate particles to high energies for collision experiments
Theme 4: Astrophysics
- Stellar and Cosmic Physics
- Understand stellar formation: cloud of gas collapses under gravity; core heats and fusion begins
- Analyze stellar evolution: life cycle from formation through main sequence to death (white dwarf, neutron star, black hole)
- Understand Hertzsprung-Russell diagram: plots luminosity vs. temperature; tracks stellar evolution
- Define stellar magnitudes: apparent magnitude (as seen), absolute magnitude (intrinsic brightness); relates to distance
- Apply distance calculation: parallax and luminosity distance measure cosmic distances
- Understand galaxies: collections of billions of stars; Milky Way is spiral galaxy
- Recognize redshift: wavelengths shift toward red when objects move away; indicates recession velocity
- Understand cosmic expansion: galaxies receding from each other; universe expanding
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