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Suppose we use delta function wells, instead of spikes (i.e., switch the sign ofin Equation 5.57). Analyze this case, constructing the analog to Figure 5.6. this requires no new calculation, for the positive energy solutions (except that β is now negative; use β=-1.5 for the graph), but you do need to work out the negative energy solutions (letk-2mE/handZ-ka,forE<0) and , for). How many states are there in the first allowed band?

Short Answer

Expert verified

The states in first allowed band are

If E>0thencosKa=coska-h2ksinkaIfE<0thencosKa=coshka-h2ksinhka

Step by step solution

01

Define the Schrodinger equation

  • A differential equation that describes matter in quantum mechanics in terms of the wave-like properties of particles in a field. Its answer is related to a particle's probability density in space and time.
  • The time-dependent Schrodinger equation is represented as

02

Finding the states in the band

Consider two cases, when particle has positive energy (E > 0) and when it has negative energy(E>0)

i) E>0: Here αis negative:

cosKa=coska-mαh2ksinkak=2mEh2,K=2πnNa

(ii) E>0First write Schrodinger equation for region 0<x<a-ħ22m2ψx2=-E

2ψx2=2mEħ2ψ=kψ

Since k is positive, solution is

ψlx=Acoshkx+Bsinhkx

Using Bloch’s theorem, wave function in the “cell” to the left of the origin (in the region ),-a<x<0),isψllx=e-ikaAcoshkx+a+Bsinhkx+a

03

Calculating the first derivation

Now we impose boundary conditions, at x=0 wave function must be continuous but its deviation isn’t because of delta potential.A=e-ikaAcoshka+Bsinhka

To find the derivation of wave function in point x=0 , we write Schrodinger equation:

-h22m2ψx2-αδxψ=-Eψ

To find first derivation we need to integrate previous equation from-ε to +ε. After taking the limit ε0, RHS of equation vanishes, and we are left with:

h22m[ψx]x0+-[ψx]x0-=-αψ0[ψlx]x=0-[ψllx]x=0=-2mαh2ψ0Bk-e-iKa(Asinhka+Bcoshka)=-2mαh2A

04

Calculating the value of B

B=AeiKa-coshħasinhka

Result in expression about it

Akeika-coshka-ke-ikaAsinh2ka+Aeikacoshka-Acosh2ka=-2mαAh2sinhkakeika-kcoshka-ke-ikaeikacoshka-1=-2mαAh2sinhkakeika-2kcoshka-2mαAh2sinhka2mαħ2sinhkacosKa=coshka-mαh2ksinhka

In order to graph this function, we introduce substitute:

z=-ka,β=-mαaħcoska=fz=coshz+βsinhzz

Because must be in region between and 1 that means:

Ka=2πnNa,n=0,1,2,...,N-1

Every band has N states.

Therefore the states in first allowed band are

role="math" localid="1658232648734" IfE>0thencosKa=coska-h2ksinkaIfE<0thencosKa=coshka-h2ksinka

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Most popular questions from this chapter

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?

(a) Construct the completely anti symmetric wave function ψ(xA,xB,xC)for three identical fermions, one in the state ψ5, one in the state ψ7,and one in the state ψ17

(b)Construct the completely symmetric wave function ψ(xA,xB,xC)for three identical bosons (i) if all are in state ψ11(ii) if two are in state ψ19and another one is role="math" localid="1658224351718" ψ1c) one in the state ψ5, one in the state ψ7,and one in the stateψ17

(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%?

Find the average energy per free electron (Etot/Nd), as a fraction of the

Fermi energy. Answer:(3/5)EF

Suppose you have three particles, and three distinct one-particle stateΨaX,ΨbX,andΨcxare available. How many different three-particle states can be constructed (a) if they are distinguishable particles, (b) if they are identical bosons, (c) if they are identical fermions? (The particles need not be in different states -ΨaX1,ΨaX2Ψax3would be one possibility, if the particles are distinguishable.)

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