ASTR 1020 1st Edition Lecture 6 Outline of Last Lecture I. The SunA. PropertiesB. Nuclear EnergyC. Energy Transport in Solar Interior Outline of Current Lecture I. The Sun: Our StarA. NeutrinosB. Solar AtmosphereC. Sun SpotsD. CoronaCurrent LectureI. The SunA. Neutrinos- Neutrinos created during fusion fly directly through the Sun- Observations of these solar neutrons can tell what’s happening in the core.- Sudbury Neutrino Observatory (built 6800 feet underground): Neutrinos reacted with the heavy water to produce flashes of light (Cherenkov radiation) detected by an array of 9600 photomultiplier tubes. Right amount, but some have changed forms.B. Solar Atmosphere- Photosphere (opaque limit)- Chromosphere (hotter, 6000K- Corona (really hot, 1,000,000K)- Solar wind (extends through solar system)- All subject to activity- Diagram: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 substitute.C. Sun Spots- Cooler than other parts of the Sun’s surface (4000K)- Regions with strong magnetic fields- Diagram: - Zeeman Effect: Magnetic fields in sunspots observed by the splitting of spectral lines- Loops of bright gas often connect sunspot pairs. Magnetism and gas motion heat upper levels- Magnetic activity also causes solar prominences that erupt high above thesun’s surface.- Magnetic activity causes solar flares that send fast bursts of x-rays and charged particles into space.D. Corona- Appears bright in x-ray photos in places where magnetic fields trap hot gas- Coronal mass ejections send bursts of energetic charged particles out through the solar
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