Lecture 19: Extreme Stars: White Dwarfs & Neutron Stars
Update: 2006-01-31
Description
What happens to the cores left behind at the end of a star's life?
This lecture introduces these stellar remnants: White Dwarfs
(remnants of low-mass stars held up by Electron Degeneracy Pressure),
and Neutron Stars (remnant cores of core-bounce supernovae held up
by Neutron Degeneracy Pressure). We also the Chandrasekhar Mass for
White Dwarfs, Type Ia Supernovae resulting from a white dwarf getting
tipped over the Chandrasekhar Mass, Pulsars (rapidly rotating magnetized
neutrons stars), and ask what happens when a neutron star gets tipped
over its mass limit.
Recorded 2006 January 31 in 1008 Evans Laboratory on the Columbus campus
of The Ohio State University.
This lecture introduces these stellar remnants: White Dwarfs
(remnants of low-mass stars held up by Electron Degeneracy Pressure),
and Neutron Stars (remnant cores of core-bounce supernovae held up
by Neutron Degeneracy Pressure). We also the Chandrasekhar Mass for
White Dwarfs, Type Ia Supernovae resulting from a white dwarf getting
tipped over the Chandrasekhar Mass, Pulsars (rapidly rotating magnetized
neutrons stars), and ask what happens when a neutron star gets tipped
over its mass limit.
Recorded 2006 January 31 in 1008 Evans Laboratory on the Columbus campus
of The Ohio State University.
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