2.12 Astro 1

2.12 Astro 1 - Astro 1 Section 1 Professor Brandt Friday...

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Astro 1 Section 1 Professor Brandt Friday February 12th 1999 Announcements: Lecture notes: Class 15. In the last class we talked about the life of a star like our sun - will review and stress new points. 1 M (.) star. Proto Star - contracting from gas cloud. No fusion. Takes 30 million years. Main Sequence - has a core that burns H->He. 10 Billion years. Surface temp is 6000K. Core is 15 million K. Orange and Red Giants - core contracts while envelope swells up. He -> C burning starts in core. H->He in shell. But carbon never starts fusion burning. Needs 600 million K to burn Carbon - not enough gravity so core never gets hot enough. Carbon core is very dense. 1 grape of it would weigh 1 ton. Planetary nebula - violent burning inside ejects envelope into space. White dwarf - Ultra dense carbon core left over - > dead star with no fusion. Now gravity still squeezes core - always before energy from fusion burning has fought off gravity. But now no fusion. How does a star stay up? Quantum mechanical effect called electron degeneracy
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This note was uploaded on 02/20/2008 for the course ASTRO 1 taught by Professor Brandt during the Spring '99 term at Penn State.

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2.12 Astro 1 - Astro 1 Section 1 Professor Brandt Friday...

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