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Our Sun. http://www.nasa.gov/images/content/524990main_FAQ10_full.jpg. How did it form? Basic facts 99.8% of mass 100x diameter of Earth 5,527 o C 92.1% H, 7.8% He Plasma Sun today Main source of Earth’s energy. How do we get the Sun’s energy?. Need to know! Thermal energy - PowerPoint PPT Presentation
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How did it form? Basic facts
99.8% of mass 100x diameter of Earth 5,527oC 92.1% H, 7.8% He Plasma Sun today Main source of Earth’s
energy
Our Sun
http://www.nasa.gov/images/content/524990main_FAQ10_full.jpg
Need to know! Thermal energy Temperature Heat
3 Types of heat Occur in different parts of the Sun1. Conduction
Core Dense, hottest
Hydrogen fusion
How do we get the Sun’s energy?
Light waves How energy gets to Earth
Radiation Zone Energy moves slowly
Thick layer
2. Radiation
3. Convection
In liquids and gases Material heated
(conduction) Rises….why? Sinks….why? Repeat
Convection Zone Moves more
quickly in this layer
Inner Solar Structure Review
Core
Radiation Zone
Convection Zone
Photosphere Visible surface
Chromosphere Temp. increases Red glow
Corona Outermost layer Very hot Seen during an eclipse
Outer Solar Structure
What is a magnetic field?
What causes a magnetic field? On the Sun?
Effect of rotation Different rotation rates Magnetic field lines get
wound up Eventually snap
Sun’s Magnetic Field
http://www.cbsnews.com/8301-205_162-57597396/
Intense magnetic field prevents convection.
Cooler than nearby areas Appear in pairs Brightness & temp.
Sunspots
http://oneminuteastronomer.com/1018/sunspots/
Predictable cycle 11-years Minimums
Last = 2008/2009
Low # of prominences, flares and sunspots
Cooler climate on Earth
Last maximum = 2013
Sunspot Cycle
http://academic.emporia.edu/aberjame/student/johnson5/sunspotcycle.html
Solar flares Caused by field snap High energy Explosive
Prominence Loops/arches Follow magnetic field lines into space
Surface Features
Solar Wind Plasma stream Hot, high speed
Coronal Mass Ejections (CME) Massive eruption Rearrangement of magnetic field lines Recent CMEs
Effects on Earth Disrupt magnetic field shape Damage electronics Danger to astronauts
Solar Wind & CME
http://stereo.gsfc.nasa.gov/browse/2013/10/14/index.shtml
Interaction of particles and magnetic field Particles drawn to
poles Colors
Elements Altitude
Constantly changing
Borealis or Australis
Video
Aurora
http://www.public.iastate.edu/~sdk/fick2003/october.html