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A simplified approach to the question of how lis related to angular momentum 鈥 due to P. W. Milonni and Richard Feynman 鈥 can be stated as follows: If can take on only those values mlh, whereml=0,1,l , then its square is allowed only valuesml2h2, and the average of localid="1659178449093" l2should be the sum of its allowed values divided by the number of values,2l+1 , because there really is no preferred direction in space, the averages of Lx2andLy2should be the same, and sum of all three should give the average of role="math" localid="1659178641655" L2. Given the sumrole="math" localid="1659178770040" 1Sn2=N(N+1)(2N+1)/6, show that these arguments, the average of L2 should be l(l+1)h2.

Short Answer

Expert verified

Given the sum 1Sn2=N(N+1)(2N+1)/6the average of L2isl(l+1)h2.

Step by step solution

01

Average of Lz2 :

The Azimuthal quantum number specifies the shape and angular momentum of the orbital in the space.

Given that,

If L2can take on only those values mlh, where ml=0,1,l, then its square is allowed only values ml2h2, and the average of l2 should be the sum of its allowed values divided by the number of values, 2l+1, because there really is no preferred direction in space, the averages of Lx2andLy2 should be the same, and sum of all three should give the average ofL2 .

Where, L is the Orbital angular momentum, Lx is the component of orbital angular momentum along x-axis, Ly is the component of orbital angular momentum along y-axis, Lz is the component of orbital angular momentum along z-axis, l is theAzimuthal quantum number,ml is theMagnetic quantum number.

role="math" localid="1659179529670" Lz2=12l+1ml=-llml2h2

Where, h is Planck鈥檚 constant.

Lz2=22l+1ml=-llml2h2=22l+1h2ll+12l+1/6=13h2ll+1

02

Average of  :

It is also given that,

Avg.ofLx2=Avg.ofLy2=Avg.ofLz2 鈥.. (1)

Hence,

Avg.ofL2=Avg.ofLy2=Avg.ofLz2=3Avg.ofLx2+Avg.ofLy2+Avg.ofLz2=3AvgofLz2=313h2ll+1=h2ll+1

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Most popular questions from this chapter

Consider two particles that experience a mutual force but no external forces. The classical equation of motion for particle 1 is v1=F2on1/m1, and for particle 2 is v2=F1on2/m2, where the dot means a time derivative. Show that these are equivalent to vcm=constant, and vrel=FMutual/ .Where, vcm=(m1v1+m2v2)/(m1m2),FMutual=-Fion2and=m1m2(m1+m2).

In other words, the motion can be analyzed into two pieces the center of mass motion, at constant velocity and the relative motion, but in terms of a one-particle equation where that particle experiences the mutual force and has the 鈥渞educed mass鈥 .

Some degeneracies are easy to understand on the basis of symmetry in the physical situation. Others are surprising, or 鈥渁ccidental鈥. In the states given in Table 7.1, which degeneracies, if any, would you call accidental and why?

An electron is in anI = 3state of the hydrogen atom, what possible angles might the angular momentum vector make with the z-axis.

To conserve momentum, an atom emitting a photon must recoil, meaning that not all of the energy made available in the downward jump goes to the photon. (a) Find a hydrogen atom's recoil energy when it emits a photon in a n = 2 to n = 1 transition. (Note: The calculation is easiest to carry out if it is assumed that the photon carries essentially all the transition energy, which thus determines its momentum. The result justifies the assumption.) (b) What fraction of the transition energy is the recoil energy?

Classically, an orbiting charged particle radiates electromagnetic energy, and for an electron in atomic dimensions, it would lead to collapse in considerably less than the wink of an eye.

(a) By equating the centripetal and Coulomb forces, show that for a classical charge -e of mass m held in a circular orbit by its attraction to a fixed charge +e, the following relationship holds

=er-3/240m.

(b) Electromagnetism tells us that a charge whose acceleration is a radiates power P=e2a2/60c3. Show that this can also be expressed in terms of the orbit radius as P=e696203m2c3r4. Then calculate the energy lost per orbit in terms of r by multiplying the power by the period T=2/and using the formula from part (a) to eliminate .

(c) In such a classical orbit, the total mechanical energy is half the potential energy, or Eorbit=-e280r. Calculate the change in energy per change in r : dEorbit/dr. From this and the energy lost per obit from part (b), determine the change in per orbit and evaluate it for a typical orbit radius of 10-10m. Would the electron's radius change much in a single orbit?

(d) Argue that dividing dEorbit/dr by P and multiplying by dr gives the time required to change r by dr . Then, sum these times for all radii from rinitial to a final radius of 0. Evaluate your result for rinitial=10-10m. (One limitation of this estimate is that the electron would eventually be moving relativistically).

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