ch 17 -our dynamic sun
TRANSCRIPT
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Our Dynamic Sun
You should never look directly at the sun.
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The Sun is Large
• How
• Large
• is
• It?
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http://space-facts.com/how-big-is-the-sun-million-earths/
• 1.3 million Earths will fit in the sun.
• https://www.youtube.com/watch?v=qLB5ma2Yz1I
• What is happening up there?
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Interior
• Interior: http://solarscience.msfc.nasa.gov/interior.shtml
• 1. Core: The Sun's core • is the central region • where nuclear reactions• consume hydrogen to • form helium.• Temp: 27,000,000 OF
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Here is how fusion works:
• (3) step process called proton-protonchain. (fusion)
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step one summary
• Proton + Proton
• H + H = deuterium + neutrino
• and a positron
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Gamma Ray
• When a positron collides with its • antiparticle (electron) they annihilate• to form a gamma ray.
• These gamma rays eventually make their way into space in the form of sunlight.
• neutrinos just come out and can eventually• make it to earth.
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Step Two summary:
deuterium + proton = Helium-3 nucleusand a gamma ray.
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Step Three Summary
Two Helium-3collide to forma Helium 4 nucleus and2 extra protons
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Radiative ZoneCharacterized by the factthat the energy from the core is carried by photonsthrough the radiative zone.
Because of the density, it takes a photon about a million years to finally reachthe interface layer.
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Radiative Zone
• Temperature falls to about 2,000,000 0C progressively through this zone.
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Tachocline (Interface Layer)
• This is an area that lies between the Radiative zone and the Convective Zone.
• This is where the suns magnetic field is generated.
• Thin layer with border behaviors to match each border.
• This change in fluid flow velocities gives its alternative name: Tachocline Layer.
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Convection Zone
• Outer most layer. This is the begining
• of the visible surface.
• Material is more opaque here because
• heavier ions hold onto some of their
• electrons.
• Radiation has a harder time getting through.
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Convection Zone
• So heat is trapped and the fluids start to boil. Then material starts to move
• higher and since this material is warmer
• it will rise higher until it reaches the surface.
At the visible surface the temp is about
• 5426 0C. Density is .0000002 g/cm3 .
• Convective motion is visible at the surface.
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Interior Summary
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Photosphere
• Photosphere: The • visible surface of the• sun that we are most• familiar with.
• Has sunspots, prominences, • and granules.
• http://solarscience.msfc.nasa.gov/surface.shtml
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Chromosphere
• http://solarscience.msfc.nasa.gov/chromos.shtml
An irregular layer above the photospherewhere the temperature rises from 6000°C to about 20,000°C.
At these temps Hydrogen emits red light which is seen as prominences during a solar eclipse.
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Transition Region
• The Transition Region: http://solarscience.msfc.nasa.gov/t_region.shtml
The transition region is a thin and very irregular layer of the Sun's atmosphere that separates the hot corona from the much cooler chromosphere.
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The Transition Region
Instead of hydrogen, the light emitted by the transition region is dominated by such ions as C IV, O IV, and Si IV (carbon, oxygen, and silicon each with three electrons stripped off)
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Corona
• 1. Sun’s Outer Atmosphere
• Features: Streamers, Plumes, Loops
White Light Corona – visible during eclipse.
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Corona
Emission line Corona: Hydrogen and Helium
are super heated to temps > 1,800,000°F. They are stripped of their electrons. Other elements like N, C, and O are stripped down to nuclei. These ionizedelements produce odd emission lines in a spectrum.
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Corona
X Ray Corona: The corona shines brightly in x-rays because of its high temperature. On the other hand, the "cool" solar photosphere emits very few x-rays.
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Space Weather
• The solar wind streams off of the Sun in all directions at speeds of about 400 km/s (about
• 1 million miles per hour). • The source of the • solar wind is the • Sun's hot corona. • The temperature of• the corona is so high • that the Sun's gravity • cannot hold on to it.
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Coronal Mass Ejections
• CMEs: http://www.space.com/12581-stunning-photos-solar-storms-flares-sun-weather.html
• Coronal Mass Ejections: are huge bubbles of gas threaded with magnetic field lines that are ejected from the Sun over the course of several hours
• These can cause interference with • electronics.
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More Space Weather
• Solar Wind: http://solarscience.msfc.nasa.gov/SolarWind.shtml
• Heliosphere: http://solarscience.msfc.nasa.gov/Heliosphere.shtml
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Heliosphere
• The heliosphere is a bubble in space produced by the solar wind.
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Some Interesting features
• http://www.nasa.gov/mission_pages/sdo/news/first-light.html
• The above is for SD Observatory facts from NASA and a solar prominence video.
• Solar Flare:• http://www.nasa.gov/mission_pages/sunear
th/multimedia/Solar-Events.html#.VMp13i4sCDk
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Montage
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More Montage
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And even more Montage