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The Dangers of Solar Storms and Solar Cycles 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 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 QuickTime™ and a TIFF (LZW) decompressor are needed to see this picture. http://atropos.as.arizona.edu/aiz/teaching/a250/pp.html 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 QuickTime™ and a TIFF (LZW) decompressor are needed to see this picture. 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 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 Particle radiation also emits energy Flares and coronal mass ejections release intense concentrations of energetic particles Hazardous to astronauts in orbit and satellites QuickTime™ and a TIFF (LZW) decompressor are needed to see this picture. http://www.space.com/scienceastronomy/soho_top10_winners_031125-2.html 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 What are They What Causes Them Etc. Minimums Maximums Etc. Impact on Communications Earth’s Magnetic Field Etc. Overview 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 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 Advanced Composition Explorer (ACE) What Where When Why How 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 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 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 Team Gemini