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Lecture 32: The Lives of Stars
Why do stars shine? How long do they shine? This lecture describes the
physics of stars on the main sequence, describes the mass-luminosity
relation of main sequence stars, introduces nuclear fusion power and the
nuclear fusion lifetimes of stars. From this we gain an important
insight into one of the criteria we might apply to the search for life
around other stars: we want planets around low-mass main sequence stars
that can shine more or less steadily for more that 500 Myr to 1 billion
years - maybe longer if our goal is to find intelligent life. Recorded
live on 2009 Nov 10 in Room 1005 Smith Laboratory on the Columbus campus
of The Ohio State University.
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By Richard Pogge
4.7
179179 ratings
Why do stars shine? How long do they shine? This lecture describes the
physics of stars on the main sequence, describes the mass-luminosity
relation of main sequence stars, introduces nuclear fusion power and the
nuclear fusion lifetimes of stars. From this we gain an important
insight into one of the criteria we might apply to the search for life
around other stars: we want planets around low-mass main sequence stars
that can shine more or less steadily for more that 500 Myr to 1 billion
years - maybe longer if our goal is to find intelligent life. Recorded
live on 2009 Nov 10 in Room 1005 Smith Laboratory on the Columbus campus
of The Ohio State University.
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