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Homework 12 Solution for Stellar Structure | PHYS 132, Assignments of Physics

Material Type: Assignment; Class: STELLAR STRCTR/EVOL; Subject: Physics; University: University of California - Santa Barbara; Term: Winter 2008;

Typology: Assignments

Pre 2010

Uploaded on 08/30/2009

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Phys 132 Homework 12 Solutions
Professor Crystal Martin
TA: Ellie Hadjiyska
Problem 12: (Phillips Problem 4.1)
We want to find the classical distance of closest approach of two protons with an energy of
approach equal to 2 keV. (Note: Since the rest mass of a proton is about 938 MeV, we are in the
classical regime and can use the fact that the total energy Eis equal to the Coulomb potential
energy P E at closest approach) or
E= 2 keV = e2
4π0r
or
r=1
4π0
e2
E= (8.9876 ×109N m2C2)(1.6×1019 C)2
2000 eV
1 eV
1.6×1019 J= 7.2×1013 m
or 0.0072˚
A (compare to 1˚
A size of atom) or 720 fm (compare to the 1 fm size of proton). The
probability that the two protons penetrate the barrier keeping them apart is dependent on the
Gamov energy (Phillips Eq. (4.10)) given by
EG= (παZAZB)22mrc2
where αis the fine structure constant given by
α=e2
4π0~c
1
137
For two protons, ZA=ZB= 1 and the reduced mass is given by
mr=mAmB
mA+mB
=mp
2
The Gamov energy is then
EG= (πα)2mpc2= 493 keV
The probability Pthat the two protons penetrate the Coulomb barrier (Phillips Eq. (4.12)) is
therefore
Pexp "EG
E1/2#= exp[493 keV
2 keV 1/2
] = 1.5×107
For two 4He nuclei, ZA=ZB= 2 and the reduced mass is given by
mr=mAmB
mA+mB
=mHe
22mp
pf2

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Phys 132 Homework 12 Solutions

Professor Crystal Martin TA: Ellie Hadjiyska

Problem 12: (Phillips Problem 4.1) We want to find the classical distance of closest approach of two protons with an energy of approach equal to 2 keV. (Note: Since the rest mass of a proton is about 938 MeV, we are in the classical regime and can use the fact that the total energy E is equal to the Coulomb potential energy P E at closest approach) or

E = 2 keV = e

2 4 π 0 r or

r = 1 4 π 0

e^2 E

= (8. 9876 × 109 N m^2 C−^2 ) (1.^6 ×^10

− 19 C) 2

2000 eV

1 eV

  1. 6 × 10 −^19 J

= 7. 2 × 10 −^13 m

or 0.0072˚A (compare to ∼1 ˚A size of atom) or 720 fm (compare to the ∼1 fm size of proton). The probability that the two protons penetrate the barrier keeping them apart is dependent on the Gamov energy (Phillips Eq. (4.10)) given by

EG = (παZAZB )^22 mrc^2

where α is the fine structure constant given by

α =

e^2 4 π 0 ℏc ≈^

For two protons, ZA = ZB = 1 and the reduced mass is given by

mr = mAmB mA + mB

= mp 2

The Gamov energy is then EG = (πα)^2 mpc^2 = 493 keV

The probability P that the two protons penetrate the Coulomb barrier (Phillips Eq. (4.12)) is therefore

P ≈ exp

[

EG

E

) 1 / 2 ]

= exp[

− 493 keV 2 keV

] = 1. 5 × 10 −^7

For two 4 He nuclei, ZA = ZB = 2 and the reduced mass is given by

mr = mAmB mA + mB

= mHe 2

≈ 2 mp

Plugging in, we find the Gamov energy for two 4 He nuclei to be

EG = (παZAZB )^22 mrc^2 = 64(πα)^2 mpc^2 = 64(493 keV) = 31.6 MeV

The probability for two helium nuclei with the same approach energy of 2 keV to fuse is therefore only

P ≈ exp

[

EG

E

) 1 / 2 ]

= exp

[(

31 .6 MeV 2 keV

) 1 / 2 ]

= 3 × 10 −^55 !!

This is 48 orders of magnitude lower than for the proton probability! We can see why fusion of Helium to heavier elements must wait for the core to become much hotter (such as occurs when a main sequence star’s core contracts when becoming a red giant and the core temperature increases by an order of magnitude).