How will the Sun evolve? The Sun is now a middle-aged, low-mass, Main

Sequence star in a state of hydrostatic and thermal equilibrium that has

consumed about half of the Hydrogen available for fusion in its core.

What will its subsequent evolution be as its core runs out of Hydrogen?

This lecture describes our current state of understanding of the

expected evolution of the Sun, informed by a combination of

state-of-the-art solar models and stellar evolution codes, and data

gathered from observations of nearby stars in our Galaxy. We will trace

the future history of the Sun from the present until it begins its final

phase as a fading White Dwarf some 8 Billion years in the future. Along

the way, we'll also ask what will become of Earth.

Recorded 2006 March 6 in 1008 Evans Laboratory on the Columbus campus of

The Ohio State University.

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