1. The Dangers of Solar Storms and Solar Cycles

2.  Radius = 696,000 km  Mass = 2E30 kg  Luminosity = 3.8E26 W  Rotation Rate  25 days at the equator and 30 days at the poles  Surface Temp  5,800 K average, 4,000 K sunspots

3.  Nuclear fusion is the source of all the energy released by the sun  Steady fusion rates maintain a steady luminosity  Hydrogen fusion is the primary mechanism ▪ P-P chain ▪ CNO cycle http://atropos.as.arizona.edu/aiz/teaching/a250/pp.html

4.  For every 1 million atoms of hydrogen in the entire sun  98,000 atoms of helium  850 of oxygen  360 of carbon  120 of neon  110 of nitrogen  40 of magnesium  35 of iron  35 of silicon http://webusers.astro.umn.edu/~larry/CLASS/AST2001/pre2007/massive_star_struct.jpg

5.  Plasma  Gas whose temperature is so hot it becomes sensitive to magnetism  Ionized due to high temperatures  Most energy is lost to electromagnetic radiation  Visible light  Infrared

6.  Particle radiation also emits energy  Flares and coronal mass ejections release intense concentrations of energetic particles  Hazardous to astronauts in orbit and satellites http://www.space.com/scienceastronomy/soho_top10_winners_031125-2.html

7.  Convection is an important heat transfer mechanism in the sun  Convection causes the temperature of the convection zone to remain uniform  Occurs because hot gas is less dense than cool gas

8.  What are They  What Causes Them  Etc.

9.  Minimums  Maximums  Etc.

10.  Impact on Communications  Earth’s Magnetic Field  Etc.

11.  Overview

12. Detection and Preparation  Solar and Heliospheric Observatory (SOHO)  Launch date: 1995 The Solar and Heliospheric Observatory's spectrographs and cameras have provided much of what we know about space weather and solar physics today.  Location in orbit (L1 position)  What  Where  When  Why  How

13. Detection and Preparation  Solar Terrestrial Relations Observatory (STEREO)  Launch date: 2006 A pair of satellites, the Solar Terrestrial Relations Observatory, will generate the first 3-D views of solar flares and coronal mass ejections and will predict which events threaten Earth.  What  Where  When  Why  How

14. Detection and Preparation  Advanced Composition Explorer (ACE)  What  Where  When  Why  How

15. Detection and Preparation  Solar Dynamics Observatory (SDO)  Launch date: 2008  NASA's Solar Dynamics Observatory will observe processes like convection and sunspot formation, with the goal of predicting solar storms weeks before they erupt.  What  Where  When  Why  How

16. Detection and Preparation  Solar Sentinel  Launch date: 2015  Four satellites in Solar Sentinel will fly in varying orbits around the sun, monitoring a solar storm's path all the way to Earth. A fifth orbiter will watch the far side of the sun.  What  Where  When  Why  How

17.  Basic Calculation Related to Solar Storms  Wavelength/Energy Related  Speed at which CME Travels  Something Related to 11.3 yr cycle  Nuclear Calculation  Solar Storm Magnetic Energy Required to Produce X Amps of Current in an Alaskan Pipeline  Something about Increased Corrosion Rate

18. Team Gemini