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Flashcards · YPH11 · Topic 5

Thermodynamics, Radiation, Oscillations and Cosmology flashcards

41 cards on Topic 5, subtopics 5.3 to 5.6. Pick a subtopic or study them all.

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5.3 Thermodynamics

Internal energy
The sum of the randomly distributed kinetic and potential energies of the molecules in a system.
Why does the temperature stay constant while a substance melts or boils?
The energy supplied increases the potential energy of the molecules (their separation), not their kinetic energy, so the temperature does not change.
Specific heat capacity and specific latent heat equations
ΔE = mcΔθ: energy to raise 1 kg by 1 K is c. ΔE = LΔm: energy to change the state of 1 kg with no temperature change is L.
Energy to turn 0.50 kg of water at 100 °C into steam? (L = 2.26 × 10⁶ J/kg)
E = 2.26 × 10⁶ × 0.50 = 1.13 × 10⁶ J
Absolute zero and the kelvin scale
T(K) = θ(°C) + 273. At absolute zero the molecules have minimum internal energy, not zero energy.
Ideal gas equations
pV = nRT (R = 8.31 J mol⁻¹ K⁻¹) pV = NkT (k = 1.38 × 10⁻²³ J K⁻¹) T in kelvin.
Kinetic theory: pressure, and mean molecular kinetic energy
pV = ⅓Nm⟨c²⟩ ½m⟨c²⟩ = (3/2)kT: mean molecular kinetic energy depends only on absolute temperature.
Assumptions of the kinetic model of an ideal gas
Many molecules in random motion; molecular volume negligible; no forces between molecules except in collisions; collisions elastic; collision time negligible compared with time between collisions.
Why is the internal energy of an ideal gas only kinetic?
There are no intermolecular forces, so there is no molecular potential energy. The internal energy depends only on temperature.
Core Practicals 12, 13 and 14
12: calibrate a thermistor in a potential divider as a thermostat. 13: determine a specific latent heat. 14: pressure and volume of a fixed mass of gas at constant temperature.

5.4 Nuclear Decay

Alpha radiation
A helium nucleus, charge +2. Stopped by paper. Strongly ionising.
Beta-minus radiation
An electron, charge −1. Stopped by about 3 mm of aluminium. Moderately ionising.
Gamma radiation
An electromagnetic photon, no charge. Reduced by thick lead. Weakly ionising.
Why is alpha the least penetrating radiation?
It is the most strongly ionising, so it loses its energy quickly and travels only a short distance.
Mass deficit and binding energy
Mass deficit: the mass of the separated nucleons minus the mass of the nucleus. The binding energy is ΔE = c²Δm. 1 u = 1.66 × 10⁻²⁷ kg.
Why do both fission and fusion release energy?
Binding energy per nucleon peaks around iron. Fusing light nuclei and splitting heavy nuclei both move towards higher binding energy per nucleon.
Beta-minus and beta-plus decay in terms of nucleons
β⁻: n → p + e⁻ + antineutrino (A same, Z + 1). β⁺: p → n + e⁺ + neutrino (A same, Z − 1).
Activity and the decay constant
A = λN (Bq). λ is the probability per unit time that a nucleus decays. N = N₀e^(−λt), and t½ = ln 2 / λ.
How do you find λ from activity measurements?
Subtract background, then plot ln A against t: a straight line of gradient −λ.
Core Practical 15
Investigate the absorption of gamma radiation by lead (count rate against absorber thickness, background subtracted).

5.5 Oscillations

Definition of simple harmonic motion
Acceleration is proportional to the displacement from the equilibrium position and always directed towards it: a = −ω²x. The restoring force F = −kx.
Maximum speed and maximum acceleration in SHM
v_max = ωA, at the equilibrium position. a_max = ω²A, at maximum displacement. ω = 2πf = 2π/T.
Periods of a simple pendulum and of a mass on a spring
Pendulum: T = 2π√(l/g) (small angles only). Mass–spring: T = 2π√(m/k). Neither depends on the amplitude.
A 0.60 kg mass oscillates on a spring of k = 15 N/m. Period?
T = 2π√(0.60/15) = 2π × 0.20 = 1.26 s
Phase of velocity relative to displacement in SHM
Velocity leads displacement by 90°: it is maximum at zero displacement and zero at maximum displacement.
Phase of acceleration relative to displacement in SHM
Acceleration is 180° out of phase with displacement: maximum and opposite at the extremes, zero at the centre.
Light damping
The amplitude decays gradually over many oscillations.
Critical damping
The fastest return to equilibrium without overshooting (used in car suspension). Heavy damping returns more slowly, also without oscillating.
Free vs forced oscillation, and resonance
Free: at the natural frequency with no driving force. Forced: driven by an external periodic force. Resonance: driving frequency = natural frequency, giving maximum amplitude.
Effect of more damping on a resonance curve
Lower peak amplitude, a broader curve, and the peak shifts slightly to a lower frequency.

5.6 Astrophysics and Cosmology

Newton’s law of gravitation, and the field of a point mass
F = Gm₁m₂/r² g = F/m = Gm/r²
Gravitational potential of a point mass
V = −Gm/r. Always negative, rising to zero at infinity (unlike electric potential, which can be positive).
Luminosity vs radiant flux
Luminosity L: total power emitted by a star. Radiant flux F: power received per unit area, F = L / (4πd²).
Standard candle, with an example
An object of known luminosity, so measuring its flux gives its distance. Type Ia supernovae have a consistent peak luminosity.
Trigonometric parallax
The apparent shift of a nearby star against distant background stars as the Earth orbits the Sun, used to find its distance.
Wien’s law and the Stefan–Boltzmann law
λmax T = 2.898 × 10⁻³ m K L = 4πr²σT⁴ Use Wien for temperature first, then Stefan for radius.
A star has surface temperature 5800 K. Peak wavelength?
λmax = 2.898 × 10⁻³ ÷ 5800 = 5.00 × 10⁻⁷ m (500 nm)
Hertzsprung–Russell diagram: axes and regions
Luminosity (up) against temperature (increasing to the left). Main sequence: diagonal band. Red giants: top right (cool, luminous, so large). White dwarfs: bottom left (hot, dim, so small).
Evolution of a Sun-like star and of a massive star
Sun-like: main sequence → red giant → planetary nebula → white dwarf. Massive: main sequence → red supergiant → supernova → neutron star or black hole.
Doppler red-shift equation, and the age of the universe
z = Δλ/λ ≈ v/c. Hubble’s law v = H₀d gives an age of about 1/H₀.
Why is there controversy about the age and fate of the universe?
The value of the Hubble constant is uncertain, and the possible existence of dark matter (from galactic rotation curves) and dark energy affects how the expansion changes.