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Unit 5: Thermodynamics, Radiation, Oscillations and Cosmology

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  1. 5.3 - Thermodynamics

    1. 5.3.125Heating and latent heat equations

      Be able to use the equations ΔE = mcΔθ and ΔE = LΔm

    2. 5.3.126Core Practical 12 - thermistor calibration

      CORE PRACTICAL 12: Calibrate a thermistor in a potential divider circuit as a thermostat

    3. 5.3.127Core Practical 13 - specific latent heat

      CORE PRACTICAL 13: Determine the specific latent heat of a phase change

    4. 5.3.128Internal energy

      Understand the concept of internal energy as the random distribution of potential and kinetic energy amongst molecules

    5. 5.3.129Absolute zero and molecular kinetic energy

      Understand the concept of absolute zero and how the average kinetic energy of molecules is related to the absolute temperature

    6. 5.3.130Ideal gas equation

      Be able to use the equation pV = NkT for an ideal gas

    7. 5.3.131Core Practical 14 - gas pressure and volume

      CORE PRACTICAL 14: Investigate the relationship between pressure and volume of a gas at fixed temperature

    8. 5.3.132Molecular kinetic theory equation

      Derive and use ½m⟨c²⟩ = 3kT/2 for molecular kinetic theory.

  2. 5.4 - Nuclear Decay

    1. 5.4.133Nuclear binding energy

      Understand the concept of nuclear binding energy and be able to use the equation ΔE = c2Δm in calculations of nuclear mass (including mass deficit) and energy

    2. 5.4.134Atomic mass unit

      Use the atomic mass unit (u) to express small masses and convert between this and SI units

    3. 5.4.135Nuclear fusion, fission and binding energy

      Understand the processes of nuclear fusion and fission with reference to the binding energy per nucleon curve

    4. 5.4.136Fusion conditions

      Understand the mechanism of nuclear fusion and the need for very high densities of matter and very high temperatures to bring about and maintain nuclear fusion

    5. 5.4.137Background radiation

      Understand that there is background radiation and how to take appropriate account of it in calculations

    6. 5.4.138Nuclear radiation properties

      Understand the relationships between the nature, penetration, ionising ability and range in different materials of nuclear radiations (alpha, beta and gamma)

    7. 5.4.139Nuclear equations

      Be able to write and interpret nuclear equations given the relevant particle symbols

    8. 5.4.140Core Practical 15 - gamma absorption by lead

      CORE PRACTICAL 15: Investigate the absorption of gamma radiation by lead

    9. 5.4.141Spontaneous and random nuclear decay

      Understand the spontaneous and random nature of nuclear decay

    10. 5.4.142Half-life and radioactive decay equations

      Determine half-life graphically and use A = λN, dN/dt = −λN, λ = ln 2/t½, N = N0e^(−λt), and A = A0e^(−λt), including the corresponding logarithmic equations.

  3. 5.5 - Oscillations

    1. 5.5.143Condition for simple harmonic motion

      Understand that the condition for simple harmonic motion is F = − kx, and hence understand how to identify situations in which simple harmonic motion will occur

    2. 5.5.144SHM displacement, velocity and acceleration equations

      Use a = −ω²x, x = A cos ωt, v = −Aω sin ωt, a = −Aω² cos ωt, T = 1/f = 2π/ω, and ω = 2πf for simple harmonic motion.

    3. 5.5.145SHM period equations

      Use T = 2π√(m/k) for a mass–spring oscillator and T = 2π√(l/g) for a simple pendulum.

    4. 5.5.146Displacement-time graphs for oscillations

      Be able to draw and interpret a displacement-time graph for an object oscillating and know that the gradient at a point gives the velocity at that point

    5. 5.5.147Velocity-time graphs for oscillations

      Be able to draw and interpret a velocity-time graph for an oscillating object and know that the gradient at a point gives the acceleration at that point

    6. 5.5.148Resonance

      Understand what is meant by resonance

    7. 5.5.149Core Practical 16 - unknown mass by resonance

      CORE PRACTICAL 16: Determine the value of an unknown mass using the resonant frequencies of the oscillation of known masses

    8. 5.5.150Energy conservation in oscillating systems

      Understand how to apply conservation of energy to damped and undamped oscillating systems

    9. 5.5.151Free and forced oscillations

      Understand the distinction between free and forced oscillations

    10. 5.5.152Resonance amplitude and damping

      Understand how the amplitude of a forced oscillation changes at and around the natural frequency of a system and know, qualitatively, how damping affects resonance

    11. 5.5.153Damping and plastic deformation

      Understand how damping and the plastic deformation of ductile materials reduce the amplitude of oscillation.

  4. 5.6 - Astrophysics and Cosmology

    1. 5.6.154Gravitational fields

      Understand that a gravitational field is a region where a mass experiences a force.

    2. 5.6.155Gravitational field strength

      Understand gravitational field strength g = F/m and use this relationship.

    3. 5.6.156Newton’s law of universal gravitation

      Use Newton's law of gravitation F = Gm1m2/r².

    4. 5.6.157Gravitational field due to a point mass

      Derive and use g = Gm/r² for the gravitational field due to a point mass.

    5. 5.6.158Gravitational potential in a radial field

      Use Vgrav = −Gm/r for gravitational potential in a radial field.

    6. 5.6.159Electric and gravitational fields comparison

      Be able to compare electric fields with gravitational fields

    7. 5.6.160Orbital motion

      Be able to apply Newton’s laws of motion and universal gravitation to orbital motion

    8. 5.6.161Black body radiation curves

      Understand what is meant by a black body radiator and be able to interpret radiation curves for such a radiator

    9. 5.6.162Stefan-Boltzmann law

      Be able to use the Stefan-Boltzmann law equation L = σAT4 for black body radiators

    10. 5.6.163Wien’s law

      Use Wien's law λmaxT = 2.898 × 10^−3 m K for black-body radiators.

    11. 5.6.164Radiation intensity from luminosity and distance

      Use radiation intensity I = L/(4πd²), where L is luminosity and d is distance from the source.

    12. 5.6.165Distance by trigonometric parallax

      Understand how astronomical distances can be determined using trigonometric parallax

    13. 5.6.166Distance by standard candles

      Understand how astronomical distances can be determined using measurements of intensity received from standard candles (objects of known luminosity)

    14. 5.6.167Hertzsprung-Russell diagram

      Be able to sketch and interpret a simple Hertzsprung-Russell diagram that relates stellar luminosity to surface temperature

    15. 5.6.168Hertzsprung-Russell diagram and stellar life cycles

      Understand how to relate the Hertzsprung-Russell diagram to the life cycle of stars

    16. 5.6.169Doppler effect

      Understand how the movement of a source of waves relative to an observer/detector gives rise to a shift in frequency (Doppler effect)

    17. 5.6.170Redshift and Hubble’s law

      Use redshift z = Δλ/λ ≈ −Δf/f ≈ v/c for a source moving relative to an observer, and Hubble's law v = H0d for cosmological distances.

    18. 5.6.171Age and fate of the universe

      Understand the controversy over the age and ultimate fate of the universe associated with the value of the Hubble constant and the possible existence of dark matter.