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OUR SUN

OUR SUN. The Core. Innermost layer of the sun. Density 10x that of lead. Fusion produces energy. 27 Million degrees Fahrenheit. Radiative Envelope. Transfers Energy out of the core by radiation. Convective Envelope.

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OUR SUN

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  1. OUR SUN

  2. The Core • Innermost layer of the sun. • Density 10x that of lead. • Fusion produces energy. • 27 Million degrees Fahrenheit

  3. Radiative Envelope • Transfers Energy out of the core by radiation. Convective Envelope • Transfers Energy to the outer part of the Sun by rising and falling gases..

  4. Photosphere • The visible layer of the Sun. • Location of magnetic storms • Temperature 10,000 degrees to 7,800 degrees in • sunspots. • Below Chromosphere and Corona

  5. Sunspots and Granulation

  6. Chromosphere • Location of solar flares. • Temperature 50,000 degrees. • Red in color due to an abundance of Hydrogen • Between Photosphere and Corona

  7. Chromosphere

  8. Corona • Only visible during an eclipse. • 4 million degrees Fahrenheit • Scientists are trying to figure out why it is hotter • than the other layers. • Outermost layer of the sun.

  9. Corona

  10. Infrared Corona

  11. Coronal Mass Ejections (CME’S) • A massive burst of solar wind, other light isotope plasma, and magnetic fields rising above the solar corona or being released into space. • Associated with sunspots and solar flares • Can cause strong Auroras and disrupt • radio and satellite signals.

  12. Coronal Mass Ejections (CME’S)

  13. Coronal Mass Ejections (CME’S) • During Solar maxima we see 3 CME’s a day • During Solar minima we see 1 CME every • three days

  14. How our magnetic Field protects us

  15. How our magnetic Field protects us • During solar flares and CME’s the magnetic field deflects the radiation away from the Earth’s surface

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