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IB Physics HL E 5 1 Stellar Equilibrium Questions

Explain HL stellar equilibrium as a balance between inward gravitational pressure and outward radiation pressure from fusion energy.

Syllabus
First assessment 2025
Course
Physics HL
Level
HL

Exam points

  • explain that a stable star avoids collapse when inward gravitational pressure is balanced by outward radiation pressure
  • link outward radiation pressure to energy produced by fusion in the stellar core
  • apply the pressure-balance model to explain why a star remains at approximately constant radius

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Study E.5.1—Stellar equilibrium conceptsOpen the corresponding Concept lesson for explanations, examples and exam connections.

IB Physics HL E 5 1 Stellar Equilibrium Questions question 1

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The diagram shows a simplified energy-balance model for the Earth surface-atmosphere system.

Figure for Question IB Physics HL E 5 1 Stellar Equilibrium Questions question 1 — IB Physics HL

The following data are given:

 Average albedo of Earth =0.30 Average global temperature of the surface =288 K Average Earth-Sun distance =1.5×1011 m\begin{aligned} \text { Average albedo of Earth } & =0.30 \\ \text { Average global temperature of the surface } & =288 \mathrm{~K} \\ \text { Average Earth-Sun distance } & =1.5 \times 10^{11} \mathrm{~m} \end{aligned}

The primary energy source of the Sun is the proton-proton (p-p) chain of fusion reactions. Four protons and two electrons produce a helium nucleus together with neutrinos and gamma photons. The overall reaction is:

411p+2−10e→24He+200ve+4γ4{ }_{1}^{1} \mathrm{p}+2{ }_{-1}^{0} \mathrm{e} \rightarrow{ }_{2}^{4} \mathrm{He}+2{ }_{0}^{0} v_{e}+4 \gamma

Outline the role of fusion reactions in maintaining a stable radius of the Sun.

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