L=4 R 2 T 4. Spectral Type ~ Temperature.
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Transcript of L=4 R 2 T 4. Spectral Type ~ Temperature.
![Page 1: L=4 R 2 T 4. Spectral Type ~ Temperature.](https://reader036.fdocuments.us/reader036/viewer/2022081506/5697bfac1a28abf838c9b454/html5/thumbnails/1.jpg)
max
6 nmK 109.2
λ⋅×
=T L=4R2T4
![Page 2: L=4 R 2 T 4. Spectral Type ~ Temperature.](https://reader036.fdocuments.us/reader036/viewer/2022081506/5697bfac1a28abf838c9b454/html5/thumbnails/2.jpg)
Spectral Type ~ Temperature
![Page 3: L=4 R 2 T 4. Spectral Type ~ Temperature.](https://reader036.fdocuments.us/reader036/viewer/2022081506/5697bfac1a28abf838c9b454/html5/thumbnails/3.jpg)
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![Page 5: L=4 R 2 T 4. Spectral Type ~ Temperature.](https://reader036.fdocuments.us/reader036/viewer/2022081506/5697bfac1a28abf838c9b454/html5/thumbnails/5.jpg)
• L~M3.5
![Page 6: L=4 R 2 T 4. Spectral Type ~ Temperature.](https://reader036.fdocuments.us/reader036/viewer/2022081506/5697bfac1a28abf838c9b454/html5/thumbnails/6.jpg)
Stellar Evolution
• Why is the study of stellar evolution difficult?– Stars change very little over a human lifespan, so it is impossible to
follow a single star from birth to death.
• How do we attempt to overcome this difficulty?– We observe stars at various stages of evolution, and can piece
together a description of the evolution of stars in general
– Computer models provide a “fast-forward” look at the evolution of stars.
• Mass (how much fuel is available) tells us much about how a star will evolve!
• Stellar Evolution can be viewed as a competition b/t gravity and pressure.
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1 Solar Mass Star
Fusionbegins
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The Ring Nebula
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Evolution of a high mass star
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