[00:00]	White Dwarfs
[00:01]	Stellar Death
[07:18]	Stellar Mass Function
[08:08]	Stellar Death (reprise)
[10:05]	End-States
[11:13]	White Dwarfs Physics
[16:54]	Binary Mass Transfer
[18:48]	Observing a Supernova
[20:24]	The Size of an Atom
[20:55]	A Sea of Electrons

Learning Objectives

1. Trace the passage of higher and lower mass stars through the H-R Diagram.
   • Relate the lifetime of a star on the Main Sequence inversely to its mass.
   • For high mass stars, a brief stint (millions of years) on the high end of the Main Sequence, then off to the Supergiant space, ending as neutron stars or black holes.
   • For intermediate and low mas stars, billions of years on the Main Sequence, then ascension to the Giant branch, and then a drop down to the region where white dwarfs are found.
   • Understand how Giant stars can increase in luminosity and yet decrease in temperature.

2. Determine the end-state of a stellar core from its initial mass.
   • Low mass stars (1 - 10 solar masses) become white dwarfs.
   • Intermediate mass stars (10 - 30 solar masses) become neutron stars.
   • High mass stars (more than 30 solar masses) become black holes.

3. Understand how the accretion of hydrogen from a companion object onto a white dwarf can produce a bright supernova.

4. Visualize how the strong pressure of self-gravity on an object the mass of the Sun but the size of the Earth will act to ionize the carbon and iron atoms, producing a lattice of carbon (diamonds!) and a sea of disassociated electrons.

5. Appreciate the physical beauty of white dwarfs and their surrounding gas shells.