stellar fuel, nuclear energy and elements how do stars shine? e = mc 2 how did matter come into...
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Stellar Fuel, Nuclear Energy and Elements
• How do stars shine?
E = mc2
• How did matter come into being?
Big bang stellar nucleosynthesis• How did different elements form?
Stars Supernovae• What is thermonuclear fusion ?
Synthesis of lighter atoms into heavier
ones at high temperature-density
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Nuclear Fusion: H Hep-p chain
Deuterium
Gamma-rays
neutrino
electron
positron
P.S. No gamma rays produced in the p-p reaction itself
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The Atomic and Sub-Atomic Zoo
• Atom protons, electrons neutrons
• Atomic number (#protons)
• Atomic weight (#protons+neutrons)
• Hydrogen 1H1
• Deuterium 1H2
• Same element, different nuclei isotopes
• Nuclear reactions energy
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Deuterium (Heavy Hydrogen) + Hydrogen Light Helium + gamma-rays (energy)
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Final Product H-fusion : Ordinary He + Energy
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For each layer: Weight + Pressure Above = Pressure Below
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Density and Temperature vs. Radius of Sun
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Percentage Mass and Luminosity vs. Radius of Sun
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Structure of the Sun: Three ZonesCore, Radiative, Convective
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How long with the Sun last?
• What is its current state?
• What is its mass ?
• How much does it burn?
• How old is it?
Answer: Section 9.3
• And then what?
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Future: Sun The Red Giant• When the Sun can no longer burn Hydgrogen in
the core• Core becomes helium dominated• Star expands; H-burning in outer shell• Triple-alpha nuclear reaction• Three helium nuclei carbon
• 4He2 + 4He2 + 4He2 12C6 + 2He2 + 12C6 16O8
• Helium burning Carbon/Oxygen core
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Stellar Evolution – HR Diagram
Low Mass Stars
MS RG AGB Pne WD
High Mass Stars
MS Cepheids / Supernovae
MS – Main SequenceRG – Red Giant AGB – Asymptotic Giant BranchPne – Planetary NebulaeWD – White Dwarf Sne – Supernovae
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Nucleosynthesis and Stellar Evolution of low mass stars
• Red giants continue to eject outer layers and evolve along the Asymptotic Giant Branch (AGB)
• AGB stars are left with the stellar core surrounded by a relatively thin sphere of hot gas which looks like planetary disk, and called Planetary Nebulae (PNe) (nothing to do with planets per se)
• PNe cores continue to cool and become White Dwarfs (94% stars end up as WDs)
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Nucleosynthesis in High Mass Stars
• Nuclear fusion continues beyond C/O
• For example:
12C6 + 16O8 28Si14
28Si14 + 28Si14 56Ni28 56Fe26
• Radioactive Ni Fe
• Fusion beyond iron is endothermic; does not produce energy; stars out of fuel; gravity wins and……………….
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The Supernova Onion
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The End• If the WD mass is more than 1.4 times more
massive than the Sun, it undergoes a gravitational collapse into a Neutron Star
• 1.44 M(Sun) Chandrashekhar Limit • Electrons fall into nuclei (protons)
e- + p+ no + (neutrino)• Gravitational collapse may continue; massive
stars end up as neutron stars or black holes after supernova explosion
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Cosmic Abundances
• Not yet known accurately, even in the Sun
• To wit: C, N, O abundances revised downwards by 30-50% in the last decade
• What is the Sun made of?
• Cosmic abundances relative to the Sun