AQA GCSE Physics Life Cycle of Stars and Element Formation Worksheet

What is covered

Questions and skills covered

The worksheet contains 6 pages of printable questions. A separate 6-page solutions PDF makes it easy to mark, review or share answers after the activity.

• Nebula/protostar formation through gravitational contraction and increasing central temperature
• Sustained hydrogen fusion marks the main-sequence stage, not chemical combustion with oxygen
• Main-sequence equilibrium: inward gravity opposed by outward pressure supported by fusion energy
• Initial mass rather than present radius or colour determines the broad lifecycle route
• R: red giant, hot white dwarf after outer material loss, then future cooled black dwarf
• T: red supergiant, supernova, then alternative neutron-star or black-hole remnants
• Supplied model lifetimes: 10 000 versus 8 million years; more fuel alone does not imply longer lifetime
• Hydrogen nuclei fuse to helium; a small amount of mass becomes energy of radiation
• Successive fusion can build heavier nuclei up to iron in the GCSE account
• Supernova nuclear processes can produce elements heavier than iron and eject material into space
• Production of carbon/iron distinguished from ejection, mixing and incorporation into a later planet
• R mass budget: 8.0 × 10²⁹ kg expelled, 40% of initial mass
• T initial mass is 20 Sun masses; remaining core is 1.5, so remnant mass is not initial mass
• White dwarf radiation while cooling does not prove sustained main-sequence fusion
• Six-mark-style synthesis comparing R and T; observing different stages versus following a whole lifetime in one night

About this activity

Use the stellar model to explain observational evidence, not simply recite stage labels. Distinguish initial mass, current size, nuclear production and material dispersal.

Before you start

After teaching star formation and the two stellar lifecycle routes, nuclear fusion and basic standard-form arithmetic/percentages. No A-level astrophysics required.