[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
[13:15]	Binary Mass Transfer
[15:09]	Observing a Supernova
[16:45]	The Size of an Atom
[17:16]	A Sea of Electrons

Learning Objectives

1. Trace the passage of higher and lower mass stars through the H-R Diagram.
   1. Relate the lifetime of a star on the Main Sequence inversely to its mass.
   2. 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.
   3. 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.
   4. 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.
   1. Low mass stars (1 - 10 solar masses) become white dwarfs.
   2. Intermediate mass stars (10 - 30 solar masses) become neutron stars.
   3. 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.