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TAMU ASTR 101 - The Sun
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GEOL 101 1st Edition Lecture 19Outline of Last LectureI. Why does the sun shine?II. Sun's structureIII. Nuclear fusionOutline of Current Lecture I. The Sun's energy,II. Solar activityCurrent LectureI. The Sun's energy:a. How does energy from fusion get out of the sun? --The core sends energy to a radiation zone, and finally to a convection zone where the heat is convected to the surface. Needs to spend hundreds of thousands of years in the radiation zone before it moves to the convection zone. Once heat is convected (temperature here is much lower than in the core),it only takes about 8 minutes to reach earth's surface.b. Convection= rising hot gas, takes energy to the surfacec. Granulation= little cells on the surface of the sun. Looking at the sun in a high resolution, you will see this with hot and cold regions. d. How do we know what's happening inside the Sun? --Neutrinos tells us about what's happening in the core of the sun (not the convection level or radiation level). All the energy comes from the gamma rays which make the Sun hot.II. (11.3) Solar activitya. Charged particles streaming from the Sun can disrupt electrical power grids and disable communications satellitesb. How does solar activity vary with time? --there are years where the current solar activity is extremely strong, and some years where it's extremely weak. Some people theorize that since the solar activity is currently so weak that we may be getting to a solar ice age. c. Sunspot cycle is relative to the magnetic field of the Sun.These notes represent a detailed interpretation of the professor’s lecture. GradeBuddy is best used as a supplement to your own notes, not as a


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TAMU ASTR 101 - The Sun

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