Lectures on Physics has been derived from Benjamin Crowell's Light and Matter series of free introductory textbooks on physics. See the editorial for more information....

# Atoms With More Than One Electron

What about other atoms besides hydrogen? It would seem that things would get much more complex with the addition of a second electron. A hydrogen atom only has one particle that moves around much, since the nucleus is so heavy and nearly immobile. Helium, with two, would be a mess. Instead of a wavefunction whose square tells us the probability of finding a single electron at any given location in space, a helium atom would need to have a wavefunction whose square would tell us the probability of finding two electrons at any given combination of points. Ouch! In addition, we would have the extra complication of the electrical interaction between the two electrons, rather than being able to imagine everything in terms of an electron moving in a static field of force created by the nucleus alone.

Despite all this, it turns out that we can get a surprisingly good description of many-electron atoms simply by assuming the electrons can occupy the same standing-wave patterns that exist in a hydrogen atom. The ground state of helium, for example, would have both electrons in states that are very similar to the n = 1 states of hydrogen. The second-lowest-energy state of helium would have one electron in an n = 1 state, and the other in an n = 2 states. The relatively complex spectra of elements heavier than hydrogen can be understood as arising from the great number of possible combinations of states for the electrons.

A surprising thing happens, however, with lithium, the three-electron atom. We would expect the ground state of this atom to be one in which all three electrons settle down into n = 1 states. What really happens is that two electrons go into n = 1 states, but the third stays up in an n = 2 state. This is a consequence of a new principle of physics:

 the Pauli exclusion principle Only one electron can ever occupy a given state.

There are two n = 1 states, one with sz = +1/2 and one with sz = -1/2, but there is no third n = 1 state for lithium's third electron to occupy, so it is forced to go into an n = 2 state.

It can be proved mathematically that the Pauli exclusion principle applies to any type of particle that has half-integer spin. Thus two neutrons can never occupy the same state, and likewise for two protons. Photons, however, are immune to the exclusion principle because their spin is an integer. Material objects can't pass through each other, but beams of light can, and the basic reason is that the exclusion principle applies to one but not to the other.1

 1There are also electrical forces between atoms, but as argued on page 83, the attractions and repulsions tend to cancel out.

#### Deriving the periodic table

 h / The beginning of the periodic table.

We can now account for the structure of the periodic table, which seemed so mysterious even to its inventor Mendeleev. The first row consists of atoms with electrons only in the n = 1 states:

H   1 electron in an n = 1 state

He   2 electrons in the two n = 1 states

The next row is built by filling the n = 2 energy levels:

Li   2 electrons in n = 1 states, 1 electron in an n = 2 state

Be   2 electrons in n = 1 states, 2 electrons in n = 2 states

. . .

O   2 electrons in n = 1 states, 6 electrons in n = 2 states

F   2 electrons in n = 1 states, 7 electrons in n = 2 states

Ne   2 electrons in n = 1 states, 8 electrons in n = 2 states

In the third row we start in on the n = 3 levels:

Na   2 electrons in n = 1 states, 8 electrons in n = 2 states, 1

electron in an n = 3 state

...

We can now see a logical link between the filling of the energy levels and the structure of the periodic table. Column 0, for example, consists of atoms with the right number of electrons to fill all the available states up to a certain value of n. Column I contains atoms like lithium that have just one electron more than that.

 i / Hydrogen is highly reactive. (It has been claimed recently that what exploded in the Hindenburg disaster was aluminum powder on the outside of the blimp's skin.)

This shows that the columns relate to the filling of energy levels, but why does that have anything to do with chemistry? Why, for example, are the elements in columns I and VII dangerously reactive? Consider, for example, the element sodium (Na), which is so reactive that it may burst into flames when exposed to air. The electron in the n = 3 state has an unusually high energy. If we let a sodium atom come in contact with an oxygen atom, energy can be released by transferring the n = 3 electron from the sodium to one of the vacant lower-energy n = 2 states in the oxygen. This energy is transformed into heat. Any atom in column I is highly reactive for the same reason: it can release energy by giving away the electron that has an unusually high energy.

Column VII is spectacularly reactive for the opposite reason: these atoms have a single vacancy in a low-energy state, so energy is released when these atoms steal an electron from another atom.

It might seem as though these arguments would only explain reactions of atoms that are in different rows of the periodic table, because only in these reactions can a transferred electron move from a higher-n state to a lower-n state. This is incorrect. An n = 2 electron in fluorine (F), for example, would have a different energy than an n = 2 electron in lithium (Li), due to the different number of protons and electrons with which it is interacting. Roughly speaking, the n = 2 electron in fluorine is more tightly bound (lower in energy) because of the larger number of protons attracting it. The effect of the increased number of attracting protons is only partly counteracted by the increase in the number of repelling electrons, because the forces exerted on an electron by the other electrons are in many different directions and cancel out partially.

Neutron stars, example 1

Here's an exotic example that doesn't even involve atoms. When a star runs out of fuel for its nuclear reactions, it begins to collapse under its own weight. Since Newton's law of gravity depends on the inverse square of the distance, the gravitational forces become stronger as the star collapses, which encourages it to collapse even further. The final result depends on the mass of the star, but let's consider a star that's only a little more massive than our own sun. Such a star will collapse to the point where the gravitational energy being released is sufficient to cause the reaction p + e- → n + ν to occur. (As you found in homework problem 7 on page 38, this reaction can only occur when there is some source of energy, because the mass-energy of the products is greater than the mass-energy of the things being consumed.) The neutrinos fly off and are never heard from again, so we're left with a star consisting only of neutrons!

Now the exclusion principle comes into play. The collapse can't continue indefinitely. The situation is in fact closely analogous to that of an atom. A lead atom's cloud of 82 electrons can't shrink down to the size of a hydrogen atom, because only two electrons can have the lowestenergy wave pattern. The same happens with the neutron star. No physical repulsion keeps the neutrons apart. They're electrically neutral, so they don't repel or attract one another electrically. The gravitational force is attractive, and as the collapse proceeds to the point where the neutrons come within range of the strong nuclear force (∼ 10-15 m), we even start getting nuclear attraction. The only thing that stops the whole process is the exclusion principle. The star ends up being only a few kilometers across, and has the same billion-ton-per-teaspoon density as an atomic nucleus. Indeed, we can think of it as one big nucleus (with atomic number zero, because there are no protons).

As with a spinning figure skater pulling her arms in, conservation of angular momentum makes the star spin faster and faster. The whole object may end up with a rotational period of a fraction of a second! Such a star sends out radio pulses with each revolution, like a sort of lighthouse. The first time such a signal was detected, radio astronomers thought that it was a signal from aliens.

Last Update: 2010-11-11