12.1 Rutherford’s Nuclear Model & Closest Approach
Rutherford’s alpha-particle scattering experiment showed that an atom’s positive charge and almost all of its mass are concentrated in a tiny, dense nucleus, with electrons orbiting it at a comparatively huge distance, mostly empty space.
12.1.1 Distance of closest approach
In the experiment itself (Geiger and Marsden, 1911), a narrow beam of alpha particles, helium nuclei carrying charge , was fired at a very thin gold foil. Almost all of them went straight through, but about 1 in 8000 was turned back through more than 90°. The ones that bounce almost straight back are the ones aimed dead centre at a nucleus, a head-on approach, and they let us put an actual number on how small the nucleus has to be.
Follow one such alpha particle, mass , starting far away with speed , so with kinetic energy . The target nucleus has charge , where is its atomic number (79 for gold), so the two repel. As the alpha particle closes in, that repulsion slows it down, until at some separation it stops completely for an instant, and is then pushed straight back the way it came. That turning point is the distance of closest approach.
A heavy nucleus like gold’s is about 50 times heavier than an alpha particle, so treat it as staying put. Then the total mechanical energy (kinetic plus electrostatic potential) is conserved the whole way in, and all we need to do is compare it at the start and at the turning point.
At the start, the separation is so large it might as well be infinite, so the electrostatic potential energy is zero and the energy is all kinetic:
At the turning point, the alpha particle is momentarily at rest, so its kinetic energy is zero and all of the energy has become the potential energy of the two charges and at separation , where :
Energy conservation sets the two equal:
Multiply both sides by , then divide both sides by :
or, writing out (and dividing by is the same as multiplying by ):
Reading it: a more energetic alpha particle gets closer (), and a more highly charged nucleus holds it further off (). An alpha particle that is not aimed exactly head-on gets deflected sideways before it can come this close, so is the nearest any alpha particle of that energy can reach. And since the alpha particle turns round without ever touching the nucleus, with Coulomb’s law holding all the way in, the nucleus must be smaller than : the distance of closest approach is an upper limit on the size of the nucleus.
Worked example
A 6.00 MeV alpha particle aimed head-on at a lead nucleus
An alpha particle with kinetic energy 6.00 MeV heads straight at a lead nucleus (Z = 82). How close does it get before it stops and turns back?
First convert the energy to joules (1 MeV = 10⁶ eV, and 1 eV = 1.602×10⁻¹⁹ J):
Then substitute into :
(1 fm, a femtometre or “fermi”, is 10⁻¹⁵ m.) A handy check that avoids powers of ten: , so with in MeV, , the same answer.
A lead nucleus actually has a radius of only about 7.1 fm, so the alpha particle turns back while still more than five times that distance from the centre: it never touches the nucleus at all.
12.1.2 Why the nuclear model could not be the whole story
This model had a fatal flaw: by classical electromagnetism, an electron orbiting the nucleus is constantly accelerating (circular motion), and an accelerating charge must radiate electromagnetic energy continuously. That radiated energy would come out of the electron’s orbital energy, so the electron should spiral inward and crash into the nucleus in a tiny fraction of a second. Real atoms are stable, so classical physics was missing something.
12.2 Bohr’s Postulates
12.2.1 Stationary orbits (quantised angular momentum)
Electrons can only occupy certain special circular orbits in which they do not radiate energy, called stationary states. These orbits are exactly the ones where the orbital angular momentum is an integer multiple of :
12.2.2 Photon emission and absorption
An atom emits or absorbs electromagnetic radiation only when an electron jumps from one stationary state to another, and the photon’s energy exactly equals the difference between the two states’ energies:
A jump to a lower energy state (smaller n) releases a photon (emission); a jump to a higher state (larger n) requires absorbing a photon of exactly that energy.
12.3 Deriving the Orbit Radius & Energy
Bohr’s postulates say which orbits are allowed, but not yet how big they are or how much energy the electron has in each. Both follow from combining two ingredients, one step at a time: ordinary Newtonian mechanics for an electron going round in a circle, and the angular momentum condition from §12.2.1. To keep the algebra readable, use the same as in §12.1.1, plus one more standard shorthand, (read “h-bar”), so that the quantisation condition reads simply:
Throughout, the hydrogen nucleus is a single proton with charge , taken to stay fixed (it is about 1836 times heavier than the electron), and the electron has charge and mass .
12.3.1 Step 1: The force balance
At separation , the proton pulls the electron towards itself with a Coulomb force of magnitude . To move in a circle of radius at speed , the electron needs a net inward (centripetal) force of exactly . The Coulomb pull is the only force acting on it, so it has to supply all of that:
Multiply both sides by to clear the fractions:
On its own, this is pure classical physics and allows any radius: pick an , and some speed satisfies it. It is the quantisation condition that singles out particular radii, and the next step brings the two together.
12.3.2 Step 2: Solving for the speed and the radius
The key move is to spot that the left-hand side of the force balance, , is just multiplied by one more factor of , and is exactly the quantity the postulate fixes at :
So the force balance becomes
and dividing both sides by gives the speed in the n-th orbit:
For the radius, go back to the quantisation condition and rearrange it for (divide both sides by ), then put in the speed just found:
(dividing by is the same as multiplying by its reciprocal, ). Multiplying the two fractions together:
So the speed falls as (the electron in the second orbit moves at half the speed it has in the first), while the radius grows as . The textbook writes the same result without the shorthands; putting and back in:
12.3.3 Step 3: Putting in numbers, the Bohr radius
In , everything except is a fixed constant of nature, so it pays to evaluate that part once. It is the radius of the orbit, called the Bohr radius, :
Using , , , and , work out the top and the bottom separately:
(The units do come out as metres: J² s² divided by kg × N m² C⁻² × C² reduces to m, using 1 J = 1 N m and 1 N = 1 kg m s⁻².) Every other orbit is just times this:
The same constants give the ground-state speed, :
Fast, but still under 1% of the speed of light (about ), which is why ordinary Newtonian mechanics was good enough in Step 1.
12.3.4 Step 4: Kinetic, potential, and total energy
Kinetic energy. Divide the force balance by to get , then take half of it:
Potential energy. Two point charges and at separation have electrostatic potential energy , taking zero at infinite separation. Here (proton) and (electron):
Total energy. Add the two, writing as so both terms share a denominator:
Compare the three: and . The kinetic energy is positive, the potential energy is twice as big and negative, and the total comes out negative, exactly the pattern found for a satellite in the Gravitation chapter, because both are inverse-square attractions.
12.3.5 Step 5: Substituting the radius to get the energy levels
The energy still depends on , but Step 2 says only the radii are allowed. Substitute :
(again, dividing by means multiplying by its reciprocal). The two factors of multiply to give :
In the textbook’s notation, , so this is the same as .
The fraction in front is just the size of the ground-state energy, and the quickest way to evaluate it is to notice that at the energy is , using and already worked out in Step 3:
Dividing by J per eV:
and therefore, for every level:
The negative sign reflects that the electron is bound to the nucleus; more energy is needed to free it from lower (more negative) levels. As , and : the electron is essentially free, at rest infinitely far away. That is the ionisation limit, and 13.6 eV is therefore the ionisation energy of hydrogen: the minimum energy needed to remove the electron entirely, starting from the ground state. In short: , , and .
Worked example
Everything about the n = 4 orbit, from the derived formulas
For a hydrogen electron in the n = 4 orbit, find the orbit radius, the speed, and the kinetic, potential, and total energy, then check the total against .
Radius and speed, from and :
Kinetic energy, from :
Cross-check with directly, using the speed above:
Potential energy, from , and then the total:
Exactly eV, the n = 4 entry in the table in §12.4 below. The orbit is 16 times wider than the ground-state orbit, but the electron travels round it at only a quarter of the speed.
12.4 Energy Levels & Transitions
A natural first guess is that energy levels should be evenly spaced, or even spread further apart as n increases. The opposite is true. Because , the gap between consecutive levels shrinks as n grows:
| Level n | Eₙ (eV) | Gap from level below |
|---|---|---|
| 1 | −13.6000 | — |
| 2 | −3.4000 | 10.2000 eV |
| 3 | −1.5111 | 1.8889 eV |
| 4 | −0.8500 | 0.6611 eV |
| 5 | −0.5440 | 0.3060 eV |
| 6 | −0.3778 | 0.1662 eV |
The rungs of the ladder crowd together higher up, converging toward (but never reaching, at any finite n) the ionisation limit at E = 0. See the interactive energy-level simulation for the live version, with the levels drawn at their true, shrinking-gap positions.
Worked example
Photon energy and wavelength for a transition
An electron falls from n=4 to n=2. Find the photon energy and its wavelength.
Using E(eV) = 1240/λ(nm):
This is the H-beta line, the second line of the Balmer series, visible as blue-green light.
12.5 Spectral Series
Every possible downward transition in hydrogen falls into one of several named series, grouped by which level the electron lands on:
12.5.1 Lyman series — final level n=1
Ultraviolet. Includes n=2→1, n=3→1, n=4→1, and so on.
12.5.2 Balmer series — final level n=2
The only series with visible lines (n=3→2 is red, n=4→2 is blue-green, and so on), which is why it was discovered first, historically.
12.5.3 Paschen series — final level n=3
Infrared. Includes n=4→3, n=5→3, n=6→3, and so on.
Within any one series, successive lines (n=3→2, then n=4→2, then n=5→2, …) get closer and closer together as the starting level increases, for exactly the same reason the energy levels themselves bunch up: the lines pile up toward a sharp series limit, the wavelength of a transition from down to that series’ final level.
Worked example
The Balmer series limit
Find the series limit (shortest wavelength, i.e. highest energy line) of the Balmer series.
This corresponds to a transition from down to n=2:
Every other Balmer line has a longer wavelength than this, and they crowd closer and closer to 364.7 nm as the starting level climbs higher.
12.6 Limitations of the Bohr Model
The Bohr model gives excellent agreement with experiment, but only for hydrogen and other single-electron (hydrogen-like) ions such as He⁺ or Li²⁺. The moment a second electron is present, electron-electron repulsion shifts the energy levels in ways this simple picture cannot account for. The model also offers no explanation for why angular momentum should be quantised in the first place, that had to wait for full quantum mechanics (de Broglie’s matter waves and the Schrödinger equation), and it cannot explain the finer details of spectral lines, such as their relative intensities or splitting in a magnetic field.
— From the NCERT exercises
Two of the chapter’s own exercise questions, with original worked solutions, both built directly on the results derived step by step in §12.3.
NCERT Exercise 12.4
The ground state energy of hydrogen atom is –13.6 eV. What are the kinetic and potential energies of the electron in this state?
Solution
Step 4 of §12.3 showed that in every Bohr orbit, and . With eV:
Check: eV, the total we started with.
NCERT Exercise 12.6
(a) Using the Bohr's model calculate the speed of the electron in a hydrogen atom in the n = 1, 2, and 3 levels. (b) Calculate the orbital period in each of these levels.
Solution
(a) Step 2 of §12.3 gave , and Step 3 worked out m/s:
(b) One revolution means covering the circumference at speed , so . Substituting and :
The period grows as : an orbit times longer, travelled times more slowly. The NCERT answer key lists the speeds as 2.18×10⁶, 1.09×10⁶ and 7.27×10⁵ m/s; the small differences in the last figure come only from rounding of the constants. The periods agree exactly.
