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What is the fate of our sun and other stars?
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Presentation transcript:

The Sun: Part I Please read Chapter 9 Astronomy 103 The Sun: Part I Please read Chapter 9

General Features Radius about 700,000 km, 100 times radius of Earth Composition: 3/4 hydrogen, about 1/4 helium by mass (90% of the atoms are hydrogen) Density: Roughly the density of water (1.4 times the density of water: 1.4 g/cm3 or 1400 kg/m3) Temperature very high at center (over 15 million K), dropping to 6,000 K near surface

Energy from the Sun Source: Wikipedia (http://en.wikipedia.org/wiki/Solar_energy)

Solar convection Figure 7.2: (b) This model explains granulation as the tops of rising convection currents just below the photosphere. Heat flows upward as rising currents of hot gas and sinking currents of cool gas. The rising currents heat the solar surface in small regions that we see as granules.

Solar wind and Aurorae Borealis http://soho.nascom.nasa.gov/classroom/nordlys_english.mp4

Solar rotation 2014 (20140101 – 20141001) compiled from SDO/HMI Quicklook data

A solar prominence observed from Solar Dynamics Observatory (SDO) https://www.youtube.com/watch?v=3Ghaf2du-XM

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