This course addresses the late stages of stellar evolution, with focus on the massive stars which end their lives
as supernovae and/or gamma ray bursts. The theory and stages of nuclear burning from helium ignition to the
formation of an iron core are laid out, and the origin the elements in the periodic table is discussed. The
important role of neutrino cooling for the now more rapid and qualitatively different stellar evolution is
emphasized. The connection between stellar properties, such as mass and metallicity, and observational
classifications are discussed in the context of the supernova that results.
The course further treats the physics of supernova explosions, and how advanced computer simulations have
improved our understanding of these. We review the fundamental processes forming the light curve and
spectra of the supernova, and diagnostic methods to determine the structure of the ejecta. Results from theory
and observations are combined to describe the landscape of successful explosions versus failed ones leading
to black hole formation, and associations between different stellar classes and supernova types.
Gamma ray bursts are reviewed, and the connection of these to the most massive and rapidly rotating stars in
the Universe is discussed. We study also briefly exotic transients such as superluminous supernovae and
kilonovae. Learnining outcomes: - describe the star's late evolutionary stages, both on microphysical and macrocopic scales, as
well as the connection between stellar properties and observational classes.
- use publicly available software to make simulations of a star’s evolution, and analyse how
changed assumptions affect the evolution.
- account for the different phases in a supernova explosion, observational properties of supernovae, and
classifications based on these properties.
- deduce and apply analytic formulae to estimate the physical parameters of a supernova from observed light
curves and spectra.
- describe fundamental phenomenology of gamma-ray bursts, models for their emission processes, and
relation to the central engine.
- couple together results from observations, simulations, and theory to differentiate between well established
and more speculative properties of massive stars, supernovae, and gamma ray bursts.
- argue for the origin of each element in the periodic table.
