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The Sun

The Sun. Layers of the Sun. The Core. Cannot be directly observed Theoretical studies of the energy it radiates Extremely hot, dense gas Plasma Density of 160,000 Kg/m3 Temperature of 1.5 x 10 7 Density + Temperature Nuclear Fusion EMR = gamma rays & particles.

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The Sun

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  1. The Sun

  2. Layers of the Sun

  3. The Core • Cannot be directly observed • Theoretical studies of the energy it radiates • Extremely hot, dense gas • Plasma • Density of 160,000 Kg/m3 • Temperature of 1.5 x 107 • Density + Temperature • Nuclear Fusion • EMR = gamma rays & particles

  4. Energy = Nuclear Fusion • Proton - Proton Chain matter is converted to energy • H+H+H+H =He + Energy • Mass of 4 H = 4.032 & Mass of 1 He = 4.003 • If the “lost” mass = .029, then using E = mc2 • How much E is this?

  5. How much energy? • 6 x 108 tons H per second • 4 x 106 tons to energy • H --> He • Amount of He in core is increasing • Core is getting bigger • Enough fuel to last another 5 billion years in present state • Temperature of core = 15 million K

  6. Radiative Zone • Lies between the core and convective zone. • Extends from the core outward to about 70% of the Sun's radius • Energy generated in core • Radiates outward • Electromagnetic radiation • Photons • Many stars have radiative zones

  7. Convective Zone • Above the radiative zone, below the photosphere • The temperature changes very rapidly with depth • Turbulent convection • Granular Texture • Heat energy and matter are carried outward in convection cells

  8. Convection Cells - Super Granules • Superheated “granules” rise from the radiative layer to the photosphere • Granules cool and sink

  9. Photosphere • Origin of visible (white) light • One of the coolest regions of the Sun • 6000 K • Only 0.1% of the gas is ionized • Densest part of the solar atmosphere • Appears as a disk with some dark spots. • Sunspots = magnetic fields • Bright = Hot, rising material • Dark = Cool, sinking material

  10. Chromosphere • Above the photosphere • 2500 kilometers thick • Appears as a thin reddish ring before & after a total eclipse • Spectra = Hydrogen • Plages = bright regions • Filaments = dark features (aka prominences) • Spicules = jets of plasma shooting up from supergranule boundaries

  11. Sunspots • Dark Spots on the Photosphere • Planet-sized regions • Dark = Cooler • 4,000 K vs. 5,800 K • The average sunspot would be about as bright as a full moon against a dark night sky. • Powerful magnetic fields around sunspots • Lead to solar flares • Coronal Mass Ejections = "solar storms" • Last from days to months • Sunspot Cycles • "sunspots" on other stars.

  12. Solar Flares • Huge explosions • Tangled magnetic fields • Snap like rubber bands • Emit huge bursts of EMR • X-rays, ultraviolet radiation, visible light, and radio waves • > 106 x energy volcanic explosion on Earth • Accompanied by Coronal Mass Ejections • Most common during "solar maximum"

  13. The dark area in the middle is a coronal hole. • These particles whiz by Earth about 5 days later, with a speed of about 700 kilometers per second, or 1.5 million miles per hour. • They then cause auroras or polar lights • cause interference in radio reception • mess up the navigation of birds. Coronal hole Mass ejection

  14. Development of Solar Flares - notice how they are contained within the magnetosphere of the sun, unless a coronal hole allows the material to escape

  15. Solar Flare with Earth as a reference

  16. The Corona • HOT! • 2,000,000 K • emits short wavelength EMR • Dark near the poles • coronal holes • source of the solar wind • Scattered white light --> plasma density • Large white regions = helmet streamers • solar plasma trapped by magnetic field.

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