[00:00]	Neutron Stars
[00:01]	Neutrons Stars
[10:52]	Degenerate Matter
[12:12]	Neutron Core
[20:26]	Supernova
[20:27]	Supernova Film - I
[26:14]	Supernova Film - II
[26:54]	Supernova Film - III
[30:00]	Pulsars

Learning Objectives

1. Understand the life-cycle of intermediate mass stars.
   • An initial solar nebula collapse results in an intermediate-mass star, which burns hydrogen on the Main Sequence for billions of years.
   • Once hydrogen and helium resources have been consumed, the star enters the red supergiant phase, expanding in size and luminosity but decreasing in temperature.
   • In the supernova phase, the star expels metals (carbon, oxygen, ...) into the surrounding interstellar medium, seeding future solar systems.
   • The remaining carbon, oxygen, calcium, and silicon in the core are fused together, forming a dense iron core roughly the size of the Earth.
   • The self-gravitational force is so strong that the iron atoms melt into hydrogen, and the constituent protons and electrons are forced together, forming a sea of pure neutrons and producing a core collapse supernova in which this single star briefly outshines an entire galaxy.

2. Visualize a neutron star as a star-mass object compressed into a volume the size of Las Cruces (a tablespoon of neutron star material weighs as much as a mountain).

3. Comprehend how the rotation of the neutron star will be magnified by the collapse process, just as ice skaters speed up by pulling their arms and legs inwards, producing pulsars which rotate 1,000 per second.