A2 · Paper 4 practice · Astronomy and cosmology

Measuring the Universe, with physics.

Ten original structured questions in the style of Paper 4, covering the whole of Astronomy and cosmology: luminosity and the inverse square law, standard candles, Wien's law and the Stefan-Boltzmann law for stellar radii, redshift, Hubble's law and the age of the Universe. The last questions build the full distance ladder. Each is tagged with its lessons; attempt them all, then reveal the worked solutions.

Original questions All questions on this page are original work, written in the Cambridge AS & A Level Paper 4 style. They are not from past papers. They test the same concepts and skills the syllabus rewards.
Data: c = 3.00 × 10⁸ m s⁻¹ · Wien constant = 2.90 × 10⁻³ m K · σ = 5.67 × 10⁻⁸ W m⁻² K⁻⁴ · H₀ = 2.3 × 10⁻¹⁸ s⁻¹ (≈ 70 km s⁻¹ Mpc⁻¹) · 1 Mpc = 3.09 × 10²² m · L☉ = 3.83 × 10²⁶ W · R☉ = 6.96 × 10⁸ m
Keep these straight

Flux, colour, redshift.

01
Paper 4
[7 marks]

The Sun has a luminosity of 3.83 × 10²⁶ W. The Earth orbits at a distance of 1.50 × 10¹¹ m.

(a) State what is meant by the luminosity of a star. [1]

(b) State what is meant by radiant flux intensity. [1]

(c) Calculate the radiant flux intensity received at the Earth. [3]

(d) State two assumptions made in using F = L / (4πd²). [2]

  • (a)The total power (energy per second) radiated by the star ✓
  • (b)The radiant power received per unit area (W m⁻²) ✓
  • (c)F = L / (4πd²) = 3.83 × 10²⁶ / (4π × (1.50 × 10¹¹)²) ✓✓ = 1.36 × 10³ W m⁻² ✓
  • (d)The star radiates uniformly in all directions ✓; no radiation is absorbed between the star and the observer ✓
02
Paper 4
[7 marks]

A type Ia supernova has a known luminosity of 1.0 × 10³⁶ W. In a distant galaxy, one is observed with a radiant flux intensity of 2.0 × 10⁻¹⁵ W m⁻².

(a) State what is meant by a standard candle. [1]

(b) Calculate the distance to the galaxy, in metres. [3]

(c) Convert this distance to megaparsecs (Mpc). [2]

(d) Suggest why standard candles are needed to find the distances to far galaxies. [1]

  • (a)An astronomical object of known luminosity (fixed by its type) ✓
  • (b)d = √(L / 4πF) = √(1.0 × 10³⁶ / (4π × 2.0 × 10⁻¹⁵)) ✓✓ = 6.3 × 10²⁴ m ✓
  • (c)6.3 × 10²⁴ / 3.09 × 10²² ✓ ≈ 2.0 × 10² Mpc (about 200 Mpc) ✓
  • (d)They are too far for parallax; a known luminosity lets the measured flux give the distance ✓
03
Paper 4
[6 marks]

Two stars, A and B, have the same luminosity. Star A is at distance d and star B is at distance 3d.

(a) Calculate the ratio Fₐ / F₮ of the fluxes received from them. [2]

(b) State which star appears brighter, and why. [2]

(c) A third pair have equal luminosity, but one appears 100 times brighter than the other. Find the ratio of their distances. [2]

  • (a)F ∝ 1/d², so Fₐ/F₮ = (3d / d)² ✓ = 9 ✓
  • (b)Star A ✓; it is closer, so its light is spread over a smaller sphere and the flux is greater ✓
  • (c)100 = (d₮ / dₐ)² ✓, so d₮ / dₐ = 10 (the fainter one is 10 times further) ✓
04
Paper 4
[7 marks]

The continuous spectrum of a star peaks at a wavelength of 480 nm.

(a) State Wien's displacement law. [1]

(b) Calculate the surface temperature of the star. [2]

(c) A second star appears red, with a peak at 700 nm. Calculate its surface temperature. [2]

(d) State which star is hotter, and how the colour tells you. [2]

  • (a)The peak wavelength is inversely proportional to absolute temperature: λₘₐₓT = 2.90 × 10⁻³ m K ✓
  • (b)T = 2.90 × 10⁻³ / 480 × 10⁻⁹ ✓ = 6.0 × 10³ K (6040 K) ✓
  • (c)T = 2.90 × 10⁻³ / 700 × 10⁻⁹ ✓ = 4.1 × 10³ K (4140 K) ✓
  • (d)The 480 nm star is hotter ✓; a shorter (bluer) peak wavelength means a higher temperature ✓
05
Paper 4
[8 marks]

A star has a luminosity of 4.0 × 10²⁸ W and a surface temperature of 1.0 × 10⁴ K.

(a) State the Stefan-Boltzmann law. [1]

(b) Calculate the power radiated per unit area of the star's surface. [2]

(c) Calculate the radius of the star. [3]

(d) Express this radius as a multiple of the Sun's radius. [2]

  • (a)The luminosity of a star is L = 4πσr²T⁴, where r is its radius and T its surface temperature ✓
  • (b)σT⁴ = 5.67 × 10⁻⁸ × (1.0 × 10⁴)⁴ ✓ = 5.7 × 10⁸ W m⁻² ✓
  • (c)r = √(L / 4πσT⁴) = √(4.0 × 10²⁸ / (4π × 5.7 × 10⁸)) ✓✓ = 2.4 × 10⁹ m ✓
  • (d)r / R☉ = 2.4 × 10⁹ / 6.96 × 10⁸ ✓ ≈ 3.4 R☉ ✓
06
Paper 4
[6 marks]

Two stars, X and Y, have the same radius. Star X has a surface temperature of 12000 K and star Y of 3000 K.

(a) Calculate the ratio of their peak wavelengths, λ₧/λₖ. [2]

(b) Calculate the ratio of their luminosities, L₧/Lₖ. [2]

(c) Comment on which star is more luminous and the role of temperature. [2]

  • (a)λ ∝ 1/T, so λ₧/λₖ = Tₖ/T₧ = 3000 / 12000 ✓ = 0.25 (X peaks at one quarter the wavelength) ✓
  • (b)Same r, so L ∝ T⁴: L₧/Lₖ = (12000 / 3000)⁴ = 4⁴ ✓ = 256 ✓
  • (c)X is far more luminous ✓; because L depends on T⁴, a fourfold temperature rise multiplies the output by 256 ✓
07
Paper 4
[7 marks]

A spectral line that has a laboratory wavelength of 434 nm is observed at 442 nm in the light from a galaxy.

(a) State what is meant by redshift. [1]

(b) Calculate the fractional shift Δλ/λ. [2]

(c) Calculate the speed of recession of the galaxy. [2]

(d) State the direction of motion of the galaxy and how the spectrum shows it. [2]

  • (a)An increase in the observed wavelength of spectral lines, caused by a source moving away ✓
  • (b)Δλ/λ = (442 − 434) / 434 ✓ = 8 / 434 = 0.018 ✓
  • (c)v ≈ c × Δλ/λ = 3.00 × 10⁸ × 0.018 ✓ = 5.5 × 10⁶ m s⁻¹ ✓
  • (d)Moving away from us (receding) ✓; the lines are shifted to longer wavelengths (toward the red) ✓
08
Paper 4
[8 marks]

The galaxy in question 7 recedes at 5.5 × 10⁶ m s⁻¹. Take H₀ = 2.3 × 10⁻¹⁸ s⁻¹.

(a) State Hubble's law. [1]

(b) Calculate the distance to the galaxy, in metres. [2]

(c) Convert this distance to megaparsecs. [2]

(d) Describe the graph of recession speed against distance for many galaxies, and state what its gradient represents. [3]

  • (a)The recession speed of a galaxy is proportional to its distance: v = H₀d ✓
  • (b)d = v / H₀ = 5.5 × 10⁶ / 2.3 × 10⁻¹⁸ ✓ = 2.4 × 10²⁴ m ✓
  • (c)2.4 × 10²⁴ / 3.09 × 10²² ✓ ≈ 78 Mpc ✓
  • (d)A straight line through the origin ✓; speed increases in direct proportion to distance ✓; the gradient is the Hubble constant H₀ ✓
09
Paper 4
[8 marks]

Observations show that almost all galaxies are receding, with v = H₀d. Take H₀ = 2.3 × 10⁻¹⁸ s⁻¹.

(a) Explain how Hubble's law supports the idea of an expanding Universe and the Big Bang. [2]

(b) Estimate the age of the Universe, in seconds. [2]

(c) Convert this age into years. (1 year ≈ 3.16 × 10⁷ s) [2]

(d) State one assumption made when using 1/H₀ as the age. [2]

  • (a)If every galaxy is receding, they were all closer together in the past ✓; running the expansion back gives a hot, dense origin (the Big Bang) ✓
  • (b)t ≈ 1 / H₀ = 1 / 2.3 × 10⁻¹⁸ ✓ = 4.3 × 10¹⁷ s ✓
  • (c)4.3 × 10¹⁷ / 3.16 × 10⁷ ✓ ≈ 1.4 × 10¹⁰ years (about 14 billion years) ✓
  • (d)The expansion rate (H₀) has stayed constant throughout the history of the Universe ✓✓
10
Paper 4
[9 marks]

Astronomers build a "distance ladder" using several methods together.

(a) State how each of standard candles, Wien's law and redshift contributes to studying a distant galaxy. [3]

(b) A Cepheid variable places a galaxy at 15 Mpc. Using H₀ = 70 km s⁻¹ Mpc⁻¹, calculate the expected recession speed. [2]

(c) A type Ia supernova in the same galaxy has a known luminosity and a measured flux. Explain how this independently confirms the distance. [2]

(d) Suggest why redshift, rather than standard candles, is used for the most distant galaxies. [2]

  • (a)Standard candles give the distance from known L and measured F ✓; Wien's law gives the surface temperature from the peak wavelength ✓; redshift gives the recession speed (and, via Hubble, distance) ✓
  • (b)v = H₀d = 70 × 15 ✓ = 1.05 × 10³ km s⁻¹ (1050 km s⁻¹) ✓
  • (c)With L known and F measured, d = √(L / 4πF) ✓; this is a second, independent estimate that should agree with the Cepheid distance ✓
  • (d)The most distant galaxies are too faint to resolve individual standard candles ✓; their redshift is still measurable, so Hubble's law gives the distance ✓

Mark this once you have attempted all ten questions and checked your working against the solutions. Revealing the solutions alone does not count.