The_Sun-2 - The The Sun Sun Visible Image of the Sun Our...

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Unformatted text preview: The The Sun Sun Visible Image of the Sun Our sole source of light and heat in the solar system A very common star: a glowing ball of gas held together by its own gravity and powered by nuclear fusion at its by nuclear fusion at its center. Pressure (from heat caused by nuclear caused by nuclear reactions) balances the gravitational pull toward the Suns center. This balance leads to a spherical ball of gas, called the Sun . What would happen if the nuclear reactions (burning) stopped? Main Regions of the Sun Radius = 696,000 km Solar Properties Solar Properties (100 times Earth) Mass = 2 x 10 30 kg Mass 2 x 10 kg (300,000 times Earth) Av Density = 1410 kg/m 3 Av. Density = 1410 kg/m 3 Rotation Period = 24.9 days (equator) 29.8 days (poles) Surface temp = 5780 K The Moons orbit around the The Moon s orbit around the Earth would easily fit within the Sun! Luminosity of the Sun = L SUN L SUN (Total light energy emitted per second emitted per second) ~ 4 x 10 26 W 100 billion one- megaton nuclear bombs every second! Solar constant: L SUN ! 4 " R 2 (energy/second/area at the radius of Earths orbit) The Solar Interior Helioseismology How do we know the interior How do we know the interior structure of the Sun? structure of the Sun? In the 1960s it was In the 1960s, it was discovered that the surface of the Sun vibrates like a bell Internal pressure waves reflect off the waves reflect off the photosphere Analysis of the Analysis of the surface patterns of these waves tell us about the inside of the Sun The Standard Solar Model Energy Transport within the Sun Extremely hot core - ionized gas No electrons left on atoms to capture photons - core/interior is transparent to light ( radiation zone ) Temperature falls further from core - more and more non-ionized atoms capture the photons - gas becomes opaque to light in the convection zone The low density in the photosphere makes it transparent to light - radiation takes over again Convection ! Convection takes over when the gas is too opaque for radiative energy transport....
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This note was uploaded on 10/19/2011 for the course AST 2037 taught by Professor Eikenberry during the Fall '08 term at University of Florida.

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The_Sun-2 - The The Sun Sun Visible Image of the Sun Our...

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