This is a short preview of an upcoming lecture on the evolution of solar mass stars. In this lecture, you’ll learn about the evolution of a one solar mass star, such as our sun, as it transitions from the main sequence to its final state as a white dwarf. I’ll show you how computer models predict these changes based on well-known physics. You’ll discover that the core runs out of hydrogen, leading to the star’s expansion into a red giant, reaching sizes that exceed Earth’s orbit. Eventually, the star sheds its outer layers, forming a planetary nebula, and the core becomes a white dwarf. We’ll delve into how computational simulations are used to map these changes by inputting the sun’s known parameters. You’ll see how factors like core density and composition shift over time. We start from the sun’s formation 4.5 billion years ago to its current state and project future changes using the Hertzsprung-Russell diagram. The core’s transformation into an inert helium structure significantly influences the sun’s evolution, driving it to leave the main sequence. Throughout the lecture, I’ll refer to observational data and showcase relevant simulations to illustrate these processes. SolarEvolution SunLifecycle Astrophysics StellarModels MainSequence RedGiant WhiteDwarf PlanetaryNebula SunTransformation StellarSimulation science Key themes and topics emphasized include: SolarEvolution, SunLifecycle, Astrophysics, StellarModels, MainSequence, RedGiant, WhiteDwarf, PlanetaryNebula, SunTransformation, StellarSimulation, science.