Led by Cecilia Payne-Gaposchkin
About this course
The fourteenth module of the Edexcel GCSE Astronomy course traces the full life cycles of stars. The student moves from the Messier and NGC catalogues and the Bayer naming system through the radiation–gravity balance that defines main-sequence stability, the changes to that balance through the life cycle of a Sun-like star (red giant, planetary nebula, white dwarf, black dwarf), the electron and neutron degeneracy pressures supporting compact remnants, and the very different evolutionary path of high-mass stars (red supergiant, supernova, neutron star or black hole) governed by the Chandrasekhar Limit.
It is led by Cecilia Payne-Gaposchkin, whose 1925 doctoral thesis established that stars are made overwhelmingly of hydrogen — the foundational insight on which all of stellar structure and evolution rests. Her thesis has been called "undoubtedly the most brilliant Ph.D. thesis ever written in astronomy."
The student leaves the module able to use the Messier and NGC catalogues, apply the Bayer naming system, account for hydrostatic equilibrium across stellar lifetimes, trace the principal stages and timescales of Sun-like and high-mass stellar evolution, and apply the Chandrasekhar Limit to compact-remnant outcomes.
Led by Cecilia Payne-Gaposchkin
The question
What forces hold a star together against its own gravity, what happens when those forces lose their balance, and why does a Sun-like star end as a white dwarf while a star eight times more massive ends as a neutron star or a black hole? The spec asks the student to use the Messier and NGC catalogues and the Bayer naming system, account for the radiation–gravity balance in main-sequence stars and the electron and neutron pressure–gravity balances in compact remnants, trace the life cycles of low-mass and high-mass stars through their named stages and approximate timescales, and apply the Chandrasekhar Limit to the question of stellar end-states.
Outcome
the student can use the Messier and NGC catalogues, apply the Bayer naming system, account for the radiation–gravity balance in main-sequence stars and the degeneracy pressures in compact remnants, trace the principal stages and timescales of low-mass and high-mass stellar evolution, and apply the Chandrasekhar Limit to compact-remnant outcomes. *(Edexcel 1AS0 Paper 2 — Topic 14, spec points 14.1–14.10)*
Sub-units