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E. Nuclear and quantum physics
E.5

Fusion and stars

IB Physics Syllabus

SL & HL
6 teaching hours
Syllabus concepts to know
  • E.5.1 that the stability of stars relies on an equilibrium between outward radiation pressure and inward gravitational forces
  • E.5.2 that fusion is a source of energy in stars
  • E.5.3 the conditions leading to fusion in stars in terms of density and temperature
  • E.5.4 the effect of stellar mass on the evolution of a star
  • E.5.5 the main regions of the Hertzsprung–Russell (HR) diagram and how to describe the main properties of stars in these regions
  • E.5.6 the use of stellar parallax as a method to determine the distance d to celestial bodies as given by 1 d(parsec) = p(arc‐second)
  • E.5.7 how to determine stellar radii.

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E.4 Fission

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