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The bottom image, taken at the same time, shows the Sun’s magnetic field, with the lightest and darkest areas indicating the strongest magnetic forces. right: A group of sunspots can be seen as bright areas near the horizon. 8 million degrees Fahrenheit). 62 oUr sUn Job:07-30798 Title:Race Point : Our Sun #175 Dtp:228 Page:62 the strUctUre of oUr sUn 63 Job:07-30798 Title:Race Point : Our Sun #175 Dtp:228 Page:63 The configuration of polarities for sunspots appearing in the same hemisphere at any particular instant is always the same.
The photosphere is composed of millions of granules, the very tops of convection cells where plasma at an average temperature over 6,000 degrees Celsius (10,832 degrees Fahrenheit) has risen through the convection zone and peeked out just far enough to spit visible light into the universe. After the granules release this energy, the plasma cools and falls back inward again. Each granule is about 1,000 kilometers (over 620 miles) in diameter, and each lasts about 20 minutes. The continuous coming and going of these granules gives the photosphere a constantly shifting turbulence, like the bubbling surface of a boiling stew.
The result is the same shockwave that bursts the star from the inside out. 30 oUr sUn Job:07-30798 Title:Race Point : Our Sun #175 Dtp:228 Page:30 Cassiopeia A is the remnant of a supernova that blew the star apart about 11,000 years ago. going sUpernova Once nuclear fusion is sparked, you can think of a star as existing in a constant tug-of-war. On one side is the inward force of gravity, constantly trying to compress the star into a denser and denser mass. On the other side is the outward force of fusion, creating pressure in the form of energy wanting to escape out into the universe.
Ado’s theorem by Andrew Phillips