Spherical symmetry buys a separation, and the separation reduces three dimensions to one. What is left is a radial equation with a barrier bolted on.
βJust as the solar system provided the first meaningful test of the laws of classical mechanics, the hydrogen atom provided the first meaningful test of the laws of quantum mechanics.β The atom is one electron of charge around a nucleus of charge , and to a first approximation the nucleus is heavy enough to hold still β so the whole of chapter 9 is one particle in one potential:
This section does not solve it. It sets up the machinery for any potential depending only on distance, and that machinery turns out to reduce a three-dimensional problem to a one-dimensional one.
Classically: a force with no torque
A central potential central potential A potential depending only on the distance from a fixed origin, V(r). It exerts no torque, so angular momentum is conserved, the eigenfunctions separate as R(r)Y_{l,m}(ΞΈ,Ο), and the problem reduces to one dimension in r. defined in ch. 9 β open in glossary gives a force pointing along . So the torque is identically zero, and the angular momentum is a constant vector.
Two consequences follow immediately. The motion stays in a fixed plane perpendicular to ; and the radius vector sweeps out area at a constant rate:
Drag the eccentricity up and the wedges become wildly different in shape β short and fat near the focus, long and thin far from it β while their areas stay equal to within the sampling error. That is the whole content of dA = (L/2m)Β dt, and it needs nothing about gravity: any central force gives it, because any central force exerts no torque. The areas here are measured from the drawn polygon by the shoelace formula, not asserted. The residual spread is under 0.4% even at e = 0.85.
Splitting the momentum of a planar orbit into radial and transverse parts,
the constant total energy becomes
The effective potential
Eq. (9.2) is remarkable if you read it right. It has the form of a one-dimensional energy β a kinetic term in the single variable , plus everything else lumped into an effective potential effective potential V_e(r) = l(l+1)Δ§Β²/2mrΒ² + V(r) β the true potential plus the centrifugal barrier. Radial motion behaves exactly like a one-dimensional problem in this potential, classically (Eq. 9.3) and quantum mechanically (Eq. 9.10) alike. defined in ch. 9 β open in glossary :
The extra term is the centrifugal barrier centrifugal barrier The l(l+1)Δ§Β²/2mrΒ² term in the effective potential: repulsive and singular at the origin, so it keeps every state with l > 0 away from r = 0. Only l = 0 states have appreciable density at the nucleus. defined in ch. 9 β open in glossary . Differentiating gives an outward force , which for a particle in a circle of radius at speed with is exactly β the familiar centrifugal force. So the term can be read two ways: as a repulsive potential, or as the transverse kinetic energy the particle must keep because its angular momentum cannot change.
For gravity, , this machinery gives the conic sections β circles, ellipses, parabolas, hyperbolas. Classical mechanics passed its first extraterrestrial test on planetary orbits precisely because a planetβs angular momentum dwarfs : the Earthβs is about .
Quantum mechanically: the same split
A state of definite energy has (Eq. 9.4) with
a partial differential equation in three variables. The move that tames it is to ask for a state with definite angular momentum as well as definite energy:
The result is the radial SchrΓΆdinger equation radial schrΓΆdinger equation Eq. (9.9): the one-dimensional equation β(Δ§Β²/2m)uβ³ + V_e(r)u = Eu for u(r) = rR(r), with u(0) = 0 and u(β) = 0. The grid-plus-eigh recipe of ch00 applies to it unchanged. defined in ch. 9 β open in glossary , with an effective potential that mirrors the classical Eq. (9.3) exactly:
Bound states are labelled by , the radial quantum number radial quantum number n_r = 0, 1, 2, β¦ β the number of nodes of the radial function u(r) strictly between r = 0 and r = β. More radial nodes means more radial kinetic energy, hence higher energy. defined in ch. 9 β open in glossary , which counts the nodes of between and . Three numbers therefore specify a state completely:
normalized by (Eq. 9.12).
Section 6.5's three-dimensional oscillator, whose answer we already know. The l(l+1)/2rΒ² barrier wins at small r and loses at large r, so the effective potential turns over. Raising l pushes the minimum outward as l(l+1) and makes it shallower as 1/l(l+1). Solved by the same grid β hamiltonian β eigh pipeline as every other potential on this site β because Eq. (9.9) is one-dimensional.
Parity
A state of definite energy in a central potential has one more definite property, and it has no classical analogue at all. Under reflection through the origin, , an eigenfunction either keeps its sign,
β even parity parity Whether a wave function is unchanged (even parity) or changes sign (odd parity) under reflection through the origin β x β βx in one dimension, r β βr in three. A reflection-symmetric Hamiltonian always has eigenfunctions of definite parity. For a central potential the parity is even when l is even and odd when l is odd, which is what forces the Ξl = Β±1 selection rule. defined in ch. 5 β open in glossary β or reverses it,
β odd parity. Using Table 8.1 you can check that has even parity for and and odd parity for ; in general the parity is .
Check yourself
0 / 6 answered
1.Why does a central potential guarantee that the orbit lies in a fixed plane?
In the widget, raise the eccentricity to 0.8 and step through the wedges.
2.The wedges change shape dramatically but their areas stay equal. What does that express?
3.What makes it legitimate to look for states with definite , **and** simultaneously?
4.Why is the substitution worth making?
5.A hydrogen state has and . What does count?
6.Why does the parity of depend only on ?