In view ofProblem 5.1, we can correct for the motion of the nucleus in hydrogen by simply replacing the electron mass with the reduced mass.

(a) Find (to two significant digits) the percent error in the binding energy of hydrogen (Equation 4.77) introduced by our use of m instead of μ.

E1=-m2h2e24π'2=-13.6eV(4.77).

(b) Find the separation in wavelength between the red Balmer lines n=3n=2for hydrogen and deuterium (whose nucleus contains a neutron as well as the proton).

(c) Find the binding energy of positronium (in which the proton is replaced by a positron—positrons have the same mass as electrons, but opposite charge).

(d) Suppose you wanted to confirm the existence of muonic hydrogen, in which the electron is replaced by a muon (same charge, but 206.77 times heavier). Where (i.e. at what wavelength) would you look for the “Lyman-α” line n=2n=1?.

Short Answer

Expert verified

(a) The percent error is 0.054%

(b)λ=9.109×10-312(1.673×10-27)(6.563×10-7)m=1.79×10-10m.

(c)μ=(13.6/2)eV=6.8eV.

(d)λ=6.54×10-10m.

Step by step solution

01

(a) Finding the percent error in the binding energy of hydrogen,

From Eq. 4.77,

E1=-me2h2e4π'2=-13eV (4.77).

E1is proportional to mass, so E1E1=mμ=m-μμ=mm+MmM-MM=mM

The fractional error is the ratio of the electron mass(m) to the proton mass(M):

9.109×10-31kg1.673×10-27kg=5.44×10-4

. The percent error is 0.054% (pretty small).

02

(b) Finding the separation in wavelength between the red Balmer lines(n=3→n=2) 

From Eq. 4.94, R is proportional to m, so

R=m4πch3e24π'2=1.097×107m-1 (4.94).

1+λ1+λ=RR=μμ=-1-λ2λ1-λ=-λλ.

So (in magnitude)role="math" localid="1656065390250" λ/λ=μ/μ.Butμ=mM/m+M., where m = electron mass,

and M = nuclear mass.

μ=m2mpm+2mp-mmpm+mp=mmpm+mpm+2mp2m+2mp-m-2mp.=m2mpm+mpm+2mp=mμm+2mpλλ=μμ=mm+2mpm2mpsoλ=m2mpλh,whereisthehydrogenwavelength.1λ=R14-19=536Rλ=365R=3651.097×107m=6.563×10-7m.λ=9.109×10-3121.673×10-276.563×10-7m=1.79×10-10m.

03

(c) Finding the binding energy of positronium,

μ=mmm+m=m2,sotheenergyishalfwhatitwouldbeforhydrogen:13.6/2eV=6.8eV.
04

(d) The “Lyman-α” line (n=2→n=1)is at,

μ=mpmμmpmμ;Rμ,soRischangedbyafactormpmμmp+mμ-mpmemp+me=mμmpmememp+mμ,ascomparedwithhydrogen.Forhydrogen,1/λ=R1-1/4=34Rλ=4/31.097×107m=1.215×10-7m,andλ1/R,soformuonichydrogentheLyman-alphalineisatλ=mμmpmememp+mμ1.215×10-7m=1206.771.673×10-27+206.77×9.109×10-311.673×10-27+9.109×10-311.215×10-7m=6.54×10-10m.

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Most popular questions from this chapter

Suppose you could find a solutionψ(r1,r2,...,rz)to the Schrödinger equation (Equation 5.25), for the Hamiltonian in Equation 5.24. Describe how you would construct from it a completely symmetric function, and a completely anti symmetric function, which also satisfy the Schrödinger equation, with the same energy.

role="math" localid="1658219144812" H^=j=1Z-ħ22mj2-14πo,0Ze2rj+1214πo,0j1Ze2rj-rk (5.24).

role="math" localid="1658219153183" H^ψ=E (5.25).

(a) Find the percent error in Stirling’s approximation for z = 10 ?

(b)What is the smallest integer z such that the error is less than 1%?

We can extend the theory of a free electron gas (Section 5.3.1) to the relativistic domain by replacing the classical kinetic energy, E=p2/2m,,with the relativistic formula, E=p2c2+m2c4-mc2. Momentum is related to the wave vector in the usual way: p=hk. In particular, in the extreme relativistic limit, Epc=hck.

(a) Replace h2k2n Equation 5.55 by the ultra-relativistic expression, hck, and calculateEtotin this regime.

dE=h2k22mVπ2k2dk (5.55).

(b) Repeat parts (a) and (b) of Problem 5.35 for the ultra-relativistic electron gas. Notice that in this case there is no stable minimum, regardless of R; if the total energy is positive, degeneracy forces exceed gravitational forces, and the star will expand, whereas if the total is negative, gravitational forces win out, and the star will collapse. Find the critical number of nucleons, Nc , such that gravitational collapse occurs for N>N_{C}is called the Chandrasekhar limit.

(c) At extremely high density, inverse beta decaye-+p+n+v,converts virtually all of the protons and electrons into neutrons (liberating neutrinos, which carry off energy, in the process). Eventually neutron degeneracy pressure stabilizes the collapse, just as electron degeneracy does for the white dwarf (see Problem 5.35). Calculate the radius of a neutron star with the mass of the sun. Also calculate the (neutron) Fermi energy, and compare it to the rest energy of a neutron. Is it reasonable to treat a neutron star non relativistic ally?

Evaluate the integrals (Equation5.108 and 5.109) for the case of identical fermions at absolute zero. Compare your results with equations 5.43 and5.45. (Note for electrons there is an extra factor of 2 in Equations 5.108 and 5.109. to account for the spin degeneracy.)

Find the energy at the bottom of the first allowed band, for the caseβ=10 , correct to three significant digits. For the sake of argument, assume αa=1eV.

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