The Sun Abundance of Elements in the Sun Element% by Number% by Mass Hydrogen92.073.4 Helium 7.825.0...
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![Page 1: The Sun Abundance of Elements in the Sun Element% by Number% by Mass Hydrogen92.073.4 Helium 7.825.0 Carbon0.02 0.20 Nitrogen0.008 0.09 Oxygen0.06 0.8.](https://reader033.fdocuments.us/reader033/viewer/2022051417/5697bfc61a28abf838ca750c/html5/thumbnails/1.jpg)
The Sun
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Abundance of Elements in the Sun
Element % by Number % by MassHydrogen 92.0 73.4
Helium 7.8 25.0
Carbon 0.02 0.20
Nitrogen 0.008 0.09
Oxygen 0.06 0.8
Neon 0.01 0.16
Magnesium 0.003 0.06
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Relative sizes
Visible sphere of the Sun
Earth
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Structure of the Sun
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What Makes the Sun to Shine?
Chemical Would only provide the necessary energy
for 3000 years
Gravitational Contraction Proposed by Helmholtz and Kelvin - would
power the Sun for a few hundred million years
By the early 1900’s geologists showed that the Earth is billions of years old.
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Nuclear Energy
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Fundamental Forces
Strong Nuclear Holds the nucleus of the atom together
Electromagnetic Responsible for all chemical reactions
Weak Nuclear Governs radioactive decay
Gravity
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Proton-proton chain
Step 1
1H + 1H —> 2H + e+ + neutrino
Step 2
2H + 1H —> 3He + photon
2He+
3He
photon
4He
photon
1H
1H
Step 3
3He + 3He —> 4He +1H + 1H +photon
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Hydrogen Fusion
Net result 4H --> He + e+ + + energy
Four protons are 0.7% more massive than one He
E = mc2
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1.6 km
C2Cl4
Neutrino Telescope
Cosmic Rays
Ar
Argon Atom
100,000 gal. tank
Gold MineAr
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Solar Neutrino Problem
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Animation
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Energy Transport
Conduction: the transfer of heat in a solid by collisions between atoms and/or molecules. Not applicable in stars
Radiation: the transfer of energy by electromagnetic waves. Inside the Sun and most stars, radiation is the principal means of heat transport.
Convection: the transfer of heat in a gas or liquid by means of the motion of the material.
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McMath-Pierce Solar Telescope
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Photosphere
Big Bear Solar Observatory
October 21, 2009
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The Sharp Limb
Limit of resolution is one arcsec 700 km at 1 AU
Density falls very quickly in photosphere
Opaque here
Transparent here
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Limb Darkening
Same 700 km penetration depth Viewed at disk center, light originates
deeper Temperature falls with height in
photosphere
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Temperature of Photosphere
0
1000
2000
3000
4000
5000
6000
7000
0 500 1000
Height in Photosphere (km)
Tem
pera
ture
(K
)
Photosphere
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Solar Spectrum
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Granulation
Typically 1000 km across
Bright center, dark edge
Center moving out, edges moving in
The Movie
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Granulation Convection
Hot Cool Hot
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Chromosphere
Observing strategies During total eclipses
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Chromosphere
Using spectroheliograph
H
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Chromosphere
Supergranulation
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Chromosphere
CaII
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Spicules
Movie
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The Corona
The quiet corona
The active corona
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X-ray emission
The Movie
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Solar Wind
Distance from photosphere
VelocityAverage particle
velocity
Escape Velocity
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The Corona is Hot
The Corona is hot! X-ray emission Lines of highly ionized iron
• FeX, FeXIV, FeXV• Requires T 2,000,000 K
Coronal holes are the source of the Solar Wind
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End of Section