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OUR SUN - PowerPoint PPT Presentation


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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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Presentation Transcript
slide5

The Core

  • Innermost layer of the sun.
  • Density 10x that of lead.
  • Fusion produces energy.
  • 27 Million degrees Fahrenheit
slide6

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..
photosphere
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
chromosphere
Chromosphere
  • Location of solar flares.
  • Temperature 50,000 degrees.
  • Red in color due to an abundance of Hydrogen
  • Between Photosphere and Corona
corona
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.
coronal mass ejections cme s
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.
coronal mass ejections cme s2
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
how our magnetic field protects us1
How our magnetic Field protects us
  • During solar flares and CME’s the magnetic field deflects the radiation away from the Earth’s surface