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Unveiling the Sun: Structure, Energy, and Phenomena

Discover the Core, Radiative Zone, and Convective Zone of the Sun. Learn about Solar Energy, Matter Conversion, and Features like Limb Darkening and Sunspots. Unravel the mystery of the Sun's immense energy output and deep layers.

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Unveiling the Sun: Structure, Energy, and Phenomena

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  1. Structure of the Sun www.assignmentpoint.com

  2. Structure of the Sun • Core: 0-20% of radius. Energy produced by nuclear fusion • Radiative Zone: 20-70% of radius: Energy travels as thermal radiation • Tachocline: Boundary of Radiative Zone: Exterior slips over interior • Convective Zone: Outer 30% of Sun: Energy moves by convection www.assignmentpoint.com

  3. Core of the Sun • Energy output: 90 billion megatons/second • Energy output = 6 microwatts/kg – less than a candle • Human body outputs 1.2 W/kg – 200,000 times greater • By volume: Core of Sun = 0.9 W/m3; Human body = 1200 W/m3. • Trying to duplicate sun’s energy output not practical on Earth; We try to use other fusion processes • Energy takes 10,000 – 100,000 years to reach surface www.assignmentpoint.com

  4. Solar Energy • 4 H  He • 4H = 4 x 1.00794 = 4.03176 • He = 4.002602 • Difference = 0.029158 = 0.7% = 1/140 • Converted to energy via E=mc2 • Once you get over being freaked out by Einstein, this is middle school math www.assignmentpoint.com

  5. Solar Energy • E=mc2 • m = kg • c = m/sec = 300,000,000 • E = joules (one Watt = 1 J/sec) • Sun’s energy output = 3.8 x 1026 W • How much mass is that per second? • m = E/c2 = 3.8 x 1026/(300,000,000)2 = 4 billion kg/sec www.assignmentpoint.com

  6. Solar Energy • Sun converts 4 billion kg of matter to energy every second • Matter conversion = 1/140 of original mass • Sun converts 560 billion kg of H to He (5.6 x 1011 kg) every second • Mass of Sun: 2 x 1030 kg • 2 x 1030 kg/ 5.6 x 1011 kg/sec = 3.6 x 1018 sec = 114 billion years www.assignmentpoint.com

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  8. The Sun We Can See • Photosphere: The Visible Disk • More transparent than air • We can see a couple of hundred kilometers deep • Chromosphere • Thin cooler atmosphere • How we know what stars are made of • Corona • Very thin but very hot • Why so hot is a mystery www.assignmentpoint.com

  9. Layers Of The Sun www.assignmentpoint.com

  10. Features On The Sun • Limb Darkening • Granulation • Sunspots • Faculae • Plages: hot clouds in the Chromosphere • Flares • Prominences www.assignmentpoint.com

  11. Surface of the Sun www.assignmentpoint.com

  12. Supergranulation www.assignmentpoint.com

  13. Supergranulation www.assignmentpoint.com

  14. Sunspots and Faculae www.assignmentpoint.com

  15. Sunspots, Faculae, Limb Darkening www.assignmentpoint.com

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