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Physics 213 General Physics Lecture 26

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Page 1: Physics 213 General Physics Lecture 26. 2 Last Meeting: Nuclear Physics I Today: Nuclear Physics II, Applications Practice Problems

Physics 213General Physics

Lecture 26

Page 2: Physics 213 General Physics Lecture 26. 2 Last Meeting: Nuclear Physics I Today: Nuclear Physics II, Applications Practice Problems

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Last Meeting: Nuclear Physics I

Today: Nuclear Physics II, Applications

Practice Problems

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Fusion in the Sun All stars generate energy through fusion The Sun, along with about 90% of other

stars, fuses hydrogenSome stars fuse heavier elements

Two conditions must be met before fusion can occur in a starThe temperature must be high enoughThe density of the nuclei must be high

enough to ensure a high rate of collisions

Page 11: Physics 213 General Physics Lecture 26. 2 Last Meeting: Nuclear Physics I Today: Nuclear Physics II, Applications Practice Problems

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Proton-Proton Cycle The proton-proton cycle

is a series of three nuclear reactions believed to operate in the Sun

Energy liberated is primarily in the form of gamma rays, positrons and neutrinos

21H is deuterium, and

may be written as 21D

1 1 21 1 1

1 2 31 1 2

1 3 41 2 2

3 3 4 12 2 2 12

H H H e

H H He

Then

H He He e

or

He He He H

Page 12: Physics 213 General Physics Lecture 26. 2 Last Meeting: Nuclear Physics I Today: Nuclear Physics II, Applications Practice Problems

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Fusion Reactors Energy releasing fusion reactions are

called thermonuclear fusion reactions A great deal of effort is being directed

at developing a sustained and controllable thermonuclear reaction

A thermonuclear reactor that can deliver a net power output over a reasonable time interval is not yet a reality

Page 13: Physics 213 General Physics Lecture 26. 2 Last Meeting: Nuclear Physics I Today: Nuclear Physics II, Applications Practice Problems

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Energy Consumption on Earth

Oil will last ~ 20-- 50 yrs, given the current rate of consumption of 7 x 1012 J/s.

Coal will last hundreds of years.Uranium (fission) will last thousands of

years.Deuterium (fusion) will last hundreds of

million of years.Solar energy (?) will last billions of years.

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(Roentgen equivalent man – same biological effectiveness as 1 Rad of x-ray)

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/ yr

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Page 20: Physics 213 General Physics Lecture 26. 2 Last Meeting: Nuclear Physics I Today: Nuclear Physics II, Applications Practice Problems

What energy must be added or given off in a reaction where two hydrogen atoms and two neutrons are combined to form a helium atom? (Atomic masses for each: hydrogen, 1.007 825 u; neutron, 1.008 665 u; helium, 4.002 602 u; also, 1 u = 931.5 MeV/c2)

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1. 10.7 MeV added

2. 10.7 MeV given off

3. 28.3 MeV given off

4. 0.931 MeV added

5. None of the above, the reaction is not possible due to conservation of energy.

Page 21: Physics 213 General Physics Lecture 26. 2 Last Meeting: Nuclear Physics I Today: Nuclear Physics II, Applications Practice Problems

If a fossil bone is found to contain 1/8th as much Carbon‑14 as the bone of a living animal, what is the approximate age of the fossil? (half‑life of 14C = 5 730 years)

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1. 2,640 years

2. 17,200 years

3. 32,900 years

4. 45,800 years

5. 60,300 years