Compact Stars

2. pressure in the core of a neutron star, we must first begin by finding the Fermi energy.
5. limit, in astrophysics, maximum mass theoretically possible for a stable white dwarf star.
6. spend billions of years fusing hydrogen to helium in their cores via the proton-proton chain.
8. are the hot, dense remnants of long-dead stars. They are stellar cores, left behind when stars exhaust their fuel supplies and blow their gases into space.
10. a type of emission nebula consisting of an expanding, glowing shell of ionized gas ejected from red giant stars late in their lives.
11. can possess exoplanets in stable orbits, some of which are closer to one star in the binary and thus orbit that star much as Earth orbits the sun, in what is called a circumstellar orbit.
12. a type of supernova that occurs in binary systems (two stars orbiting one another) in which one of the stars is a white dwarf.
14. is a quantum mechanical effect critical to understanding the stability of white dwarf stars and metal solids

1. that angular momentum will stay constant as a system changes its configuration.
3. refers collectively to white dwarfs, neutron stars, and black holes.
4. a highly magnetized rotating neutron star that emits beams of electromagnetic radiation out of its magnetic poles.
7. type of neutron star with an extremely powerful magnetic field (~10 to 10 T, ~10 to 10 G). T
9. one of the two known sets of fusion reactions by which stars convert hydrogen to helium, the other being the proton–proton chain reaction (p–p cycle),
13. is a transient astronomical event that causes the sudden appearance of a bright, apparently "new" star