IGCSE · 6 · extended response
A scale model that cannot show every scale
Space physics · Original GioPhysics question with a detailed, mark-by-mark answer guide.
- Demand
- discriminating
- Marks
- 6
- Topics
- 2
- Answer
- Complete
Parallax calibration
Supplied question data. Read the labelled axes and use the observations to test the physical model.
Vertical axis (y): Parallax / arcsec
Horizontal axis (x): Distance / pc
Read the exact data as a table
| Distance / pc | Parallax / arcsec |
|---|---|
| 5 | 0.2 |
| 10 | 0.1 |
| 20 | 0.05 |
| 40 | 0.025 |
These are the supplied values, not a worked answer. No fitted trend is drawn.
Optional enrichment: this challenge may extend beyond the usual syllabus depth and assumes confidence with algebra and graph interpretation. Use 1 AU = 1.50×10¹¹ m, solar radius = 7.0×10⁸ m and 1 parsec = 3.09×10¹⁶ m. A model puts Earth 15 m from the Sun. The supplied graph lists stellar parallax against distance; parallax p is the half-angle after Earth's six-month baseline shift, and d/pc = 1/(p/arcsec). A star has parallax 0.050 arcsec. Supplied data (Distance / pc; Parallax / arcsec): (5, 0.2), (10, 0.1), (20, 0.05), (40, 0.025).
- (a)
Find the Sun's model radius and the star's true and model distances. Explain the practical scale limitation.
3 marks - (b)
A parallax measurement has uncertainty ±0.005 arcsec. Estimate the fractional distance uncertainty and compare with a standard-candle method.
3 marks
Ready to self-mark?Reveal the detailed answer guide
(a)
Find the Sun's model radius and the star's true and model distances. Explain the practical scale limitation.
Build a chain of claim, evidence and physics reasoning. Address more than one relevant factor, identify a limitation or assumption, and finish with a conclusion that is conditional on the evidence rather than absolute.
- 1
The model scale is 15/(1.50×10¹¹) = 1.0×10⁻¹⁰, so solar radius becomes 0.070 m.
- 2
The parallax gives d = 1/0.050 = 20 pc, equal to 6.18×10¹⁷ m. Applying the same scale gives 6.18×10⁷ m, or 61800 km.
- 3
A classroom model that fits planetary orbits cannot also put the nearest stellar distances nearby at the same scale; compressed diagrams must state their distortion.
(b)
A parallax measurement has uncertainty ±0.005 arcsec. Estimate the fractional distance uncertainty and compare with a standard-candle method.
Build a chain of claim, evidence and physics reasoning. Address more than one relevant factor, identify a limitation or assumption, and finish with a conclusion that is conditional on the evidence rather than absolute.
- 1
For d = 1/p, small fractional uncertainties satisfy Δd/d≈Δp/p = 0.005/0.050 = 0.10.
- 2
The exact bounds are 1/0.055≈18.2 pc and 1/0.045≈22.2 pc, showing asymmetric inversion of the parallax limits.
- 3
A standard candle uses known luminosity and measured flux with an inverse-square model. It reaches farther than practical parallax but requires a calibrated intrinsic luminosity and corrections for absorption.
Complete marking guidance
Use these worked steps alongside the part-by-part answers. They explain the method and mark allocation; they do not add extra marks.
- The model scale is 15/(1.50×10¹¹) = 1.0×10⁻¹⁰, so solar radius becomes 0.070 m.
- The parallax gives d = 1/0.050 = 20 pc, equal to 6.18×10¹⁷ m. Applying the same scale gives 6.18×10⁷ m, or 61800 km.
- A classroom model that fits planetary orbits cannot also put the nearest stellar distances nearby at the same scale; compressed diagrams must state their distortion.
- For d = 1/p, small fractional uncertainties satisfy Δd/d≈Δp/p = 0.005/0.050 = 0.10.
- The exact bounds are 1/0.055≈18.2 pc and 1/0.045≈22.2 pc, showing asymmetric inversion of the parallax limits.
- A standard candle uses known luminosity and measured flux with an inverse-square model. It reaches farther than practical parallax but requires a calibrated intrinsic luminosity and corrections for absorption.
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