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A star converts all its hydrogen to helium, achieving a 100% helium composition. Next, it converts the helium to carbon via the triple-alpha process,

H4e+H4e+H4e→12C+7.27MeV

The mass of the star is role="math" localid="1661754478822" 4.6×1032kg, and it generates energy at the rate of 5.3x103W. How long will it take to convert all the helium to carbon at this rate?

Short Answer

Expert verified

The required time is 1.6×108yr.

Step by step solution

01

Describe the expression for the time

Let m be the mass of helium, the number of three-helium atoms in this mass equals the number of moles multiplied by the number of atoms in one mole, where the number of moles equals the mass divided by three the molar mass of the helium.

N3He=mHeNA3MHe

Let be the energy release per fusion, then the total energy released by fusion equals the number of fusions multiplied by N3He.

Efusion=N3HeQ=mHeNAQ3MHe

The energy also can be written as follows:

Efusion=PtmHeNAQ3MHe=Ptt=mHeNAQ3MHeP

02

Find the time required to convert all the helium to carbon

Substitute all the known values in equation (1).

t=4.6×1035g6.022×1023mol-17.27MeV1.602×10-13J/MeV34.0g/mol5.3×1030W=5.07×1015s=5.07×1015s3.154×107s/yr=1.6×108yr

Therefore, the required time is 1.6×108yr.

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Most popular questions from this chapter

Some uranium samples from the natural reactor site described in Module 43-3 were found to be slightly enrichedin 235U, rather than depleted. Account for this in terms of neutron absorption by the abundant isotope 238Uand the subsequent beta and alpha decay of its products.

About 2% of the energy generated in the Sun’s core by the p-p reaction is carried out of the Sun by neutrinos. Is the energy associated with this neutrino flux equal to, greater than, or less than the energy radiated from the Sun’s surface as electromagnetic radiation?

Question: Assume that immediately after the fission of U236according to Eq. 43-1, the resulting Xe140andSr94nuclei are just touching at their surfaces. (a) Assuming the nuclei to be spherical, calculate the electric potential energy associated with the repulsion between the two fragments. (Hint: Use Eq. 42-3 to calculate the radii of the fragments.) (b) Compare this energy with the energy released in a typical fission event.

In certain stars the carbon cycle is more effective than the proton–proton cycle in generating energy.This carbon cycle is

C12+H1→13N+γ,Q1=1.95MeV,N13→13C+e++v,Q2=1.19,C13+H1→14N+γ,Q3=7.55,C14+H1→15O+γ,Q4=7.30,15O→15N+e++v,Q5=1.73,C15+H1→12C+4He,Q6=4.97

(a) Show that this cycle is exactly equivalent in its overall effects to the proton–proton cycle of Fig. 43-11. (b) Verify that the two cycles, as expected, have the same Q value.

Verify the Q values reported in Eqs. 43-13, 43-14, and 43-15. The needed masses are

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