11.14.2007 - astronomy notes

11.14.2007 - astronomy notes - 11.14.2007 astronomy notes...

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11.14.2007 – astronomy notes Stellar Evolution Population snapshots Stellar physics Star-forming regions: - Cloud stability o Two forces at work: gravity (trying to collapse the cloud), heat (pressure) Numerical simulation (1 solar mass star) 1. Interstellar cloud a. Few parsecs across b. Many thousands of solar masses (typically 100,000) c. Temp: ~10K (extremely cold) d. As it collapse, it fragments e. Whole process only takes a few million years 2. One collapsing fragment a. ~ 100 solar systems across b. ~ Couple solar masses c. Contracts without much heating: low density means it is transparent radiation escapes d. ~ 30,000 years 3. Protostellar formation a. ~ 1 solar system across b. Core: density increases opaque c. Core temperature ~ 10,000 K (periphery is still cold) d. Periphery: density low, radiation escapes, temperature low disk e. ~ 100,000 years 4. Protostar a. ~ 1 mercury orbit across (still much bigger than the sun) b. Only heated due to contraction – temp goes up due to contraction
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11.14.2007 - astronomy notes - 11.14.2007 astronomy notes...

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