Lecture 12: As Long as the Sun Shines
Update: 2006-01-19
Description
How long can the Sun continue to shine, and what source of energy
does it tap to keep shining? This lecture answers this question by
introducing two important energy sources for stars: Gravitational
Contraction otherwise known as the Kelvin-Helmholz Mechanism, and
Nuclear Fusion. We will show that fusion of 4 Hydrogen nuclei into
a Helium nucleus via the proton-proton chain liberates enough energy
to provide for the Sun's Luminosity needs for about 10 Billion Years.
Recorded 2006 January 19 in 1008 Evans Laboratory on the Columbus campus
of The Ohio State University. Note: the recording mistakenly says
January 18th. Oops.
does it tap to keep shining? This lecture answers this question by
introducing two important energy sources for stars: Gravitational
Contraction otherwise known as the Kelvin-Helmholz Mechanism, and
Nuclear Fusion. We will show that fusion of 4 Hydrogen nuclei into
a Helium nucleus via the proton-proton chain liberates enough energy
to provide for the Sun's Luminosity needs for about 10 Billion Years.
Recorded 2006 January 19 in 1008 Evans Laboratory on the Columbus campus
of The Ohio State University. Note: the recording mistakenly says
January 18th. Oops.
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