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The SUN!
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Basic Facts Mass M = 2x1030 kg = 300,000ME
Radius R = 7x108 m = 7x105 km = 111RE Mean Density = Mass/Volume = M/((4/3)R3)= 1400 kg/m3 = 1.4 g/cm3 Distance = 1.5x1011 m = 1.5x108 km = 8.3 light-minutes Luminosity L = 3.9x1026 W (Solar Constant = 1350 W/m2) Mean Surface Temperature = Teffective = 5780 K Composition By Mass By Number H ~68% ~90% He ~31% ~10% “Heavies” ~1% ~1%
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The Sun Contains 99.8% of the Mass of the Entire Solar System!
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We Rely on the Sun for…
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… Source of energy Plants-photosynthesis Creates wind Water cycle
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The Sun’s Atmosphere
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Photosphere All elements are gaseous
Get denser as you move toward the core Photosphere is the “surface” we can see
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Granulation
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Chromosphere Density decreases but temperature increases
Oddity considering the rest of the sun decreases in temperature as you move away from the core
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Spicules Flamelike jets of gas that rise up into the chromosphere
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The Corona Outermost part of the Sun’s atmosphere
Extends millions of miles into space
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Reading
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Solar Activity
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Magnetic Field
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Video
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Sunspots What are they? Cause Regions marked by lower temperatures
Dark spots on the solar surface Cause Magnetic field exits one and enters the other Messes up convection in granules and causes cooling
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Structure Umbra-dark region Penumbra-lighter surrounding region
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History 1610 Sunspots were first observed by Johannes and Fabricius
1612 Galileo explained sunspots
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How They Are Used Rotation of the Sun Weather? Low sunspot activity
High sunspot activity
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Little Ice Age Low solar activity-few sunspots 1645-1715
Frozen rivers and year-round snow in unlikely places
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Sunspot Cycles Cycles every 11 years
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Maunder Minimum Lowest point of solar activity
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Prominences Magnetic field redirects the flow of the gases-out one and in the other
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Coronal Mass Ejection Causes on Earth
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Solar Winds Flow of charged particles away from the sun Continual
Greater at coronal holes and less at helmet streamers
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Fusion
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