STARS. Most of the information we have about stars comes from the study of our star, Sol aka Sun .
Our star sol
description
Transcript of Our star sol
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OUR STAR SOL
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GOALS
• You will have a basic understanding of how a star functions and how they convert matter into energy• You will discuss and write down key
vocabulary related to the structure and functions within stars
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JUST TO RECAP THE STATS WE KNOW…
• Age: 4.6 Billion years• Diameter: 1,391,000 km• Mass: 1.989 x 10^30 kg• It’s a star• It’s not on fire!!!!!
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HISTORY… OR SOMETHING LIKE IT
• The Sun was revered by many ancient peoples.
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EGYPTIANS
• The sun was revered as Ra.• Carried across the sky in a Barque (ship)• Accompanied by lesser gods for the daily
journey
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ANCIENT GREEKS
• The sun was hailed as Helios.• Carried across the sky in a chariot drawn by
fiery horses.
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ROMANS
• Celebrated the birthday of the Sun as a holiday called “Sol Invictus,” literally “Unconquered Sun.”
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MORE RECENT GREEKS
• The location of where the sun rose in the sky gave rise to the Zodiac.• It was considered a planet
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WHAT WE KNOW ABOUT THE SUN
• It is divided into 4 distinct layers• Core• Radiative Zone• Convective Zone• Photosphere• Above this is the Atmosphere of the Sun
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THE CORE
• 20-25% of the radius of the Sun• 150 x density of water• 15.7 million K• 99% of the energy in the Sun is produced
here
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DETAILS OF FUSION
• Proton-Proton fusion happens 9.7 x 10^37 times each second in the core• 6.2 x 10^11 kg /s of Helium is produced each
second in this reaction• About 1 x10^-13 x the mass of the Earth
each second or• 3.1169 x10^-19 x the Sun’s mass (slow
enough for billions of years worth of fuel)
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DETAILS OF THE FUSION CONTINUED…
• 0.7% of the mass of Helium produced is released as energy• This equates to 3.846 x 10^26 Watts of
energy per second• 4.875 x 10^24 80 Watt lightbulbs for 1
second or…• One 80 Watt bulb for 1.524 x 10^17 years
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THE RADIATIVE ZONE
• 25-70% the radius of the Sun• Temperature drops to between 7 and 2
million K
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DETAILS OF THE RADIATIVE ZONE
• Temperature gradients within the zone are to high for convection to happen• Energy is transferred by photons being
emitted and absorbed by atoms
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THE CONVECTIVE ZONE
• From about 70% of the radius of the sun to 200,000 km below its surface• Temperatures low enough that atoms are
no longer ionized• Densities low enough that convection can
occur
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CONTINUED…
• Material is heated at the surface of the radiative zone and rises up where its energy is transferred to the photosphere• Its temperature drops to 5700 K and then
sinks back to the radiative zone to be reheated
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PHOTOSPHERE
• The visible surface of the Sun• 10 to 100’s of kilometers thick• Observations of this layer resulted in the
discovery of Helium
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