Announcements Comet SWAN! Vega West. Classifying the Stars 27 October 2006.
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Transcript of Announcements Comet SWAN! Vega West. Classifying the Stars 27 October 2006.
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Announcements
Comet SWAN!
Vega
West
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Classifying the Stars
27 October 2006
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Today:
• Stellar spectra: temperatures and compositions
• Are hotter stars brighter? (H-R diagrams)
• Determining sizes of stars
• Classifying stars, looking for patterns
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Stellar Spectra
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Pleiades Spectra
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Edward Pickering and Harvard “computers,” 1890’s - 1920’s
Annie Jump Cannon
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Classifying stellar spectra
Annie Jump Cannon
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Classifying Stellar SpectraT
empe
ratu
re
“OBAFGKM”
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What are the stars made of?T
empe
ratu
re
Calcium SodiumMagnesium
Helium Hydrogen HydrogenHydrogen
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Comte quote
“We understand the possibility of determining [celestial bodies’] shapes, their distances, their sizes and motions, whereas never, by any means, will we be able to study their chemical composition.
--Auguste Comte (philosopher), 1835
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How does temperature affect spectral lines?
Cecilia Payne at Harvard, 1924
In the sun, only one H atom in a million is in level 2, ready to absorb visible light!
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The Universal Recipe of the Stars
• 74% hydrogen (by mass)
• 25% helium
• 1% other elements (for most stars)
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Are hotter stars brighter?
Plot known stars on “Hertzsprung-Russell (H-R) diagram”. Luminosity increases vertically; temperature increases to the left.
Most stars’ dots lie along a diagonal (“main sequence”), the hotter the brighter.
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H-R Diagram Patterns
Lum
ino
sity
Luminosity =
(constant) x (surface area) x (temperature)4
For a given size, hotter implies brighter.
A bright, cool star must be unusually large (“red giant”).
A faint, hot star must be unusually small (“white dwarf”).
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H-R Diagram Patterns
Most of the stars near us are fainter (and cooler) than the sun; most of the familiar stars in the night sky are brighter than the sun.
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Sizes of Main-Sequence Stars
Should be white, not green!
Hottest stars are actually somewhat larger
Reds are greatly exaggerated!
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Summary of Stellar Properties
Distance Measure using parallax (if close enough)
Velocity Proper motion and Doppler shift
LuminosityCalculate from apparent brightness and distance
Temperature From overall color or spectral class
Composition From detailed analysis of spectral lines
SizeCalculate from temperature and luminosity
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Some familiar examples