Electropaedia logo

Battery and Energy Technologies

Panel Top


End Cap
Finding your Way Around
Free Report

Buying Batteries in China

End cap



Green Cap

Woodbank does not monitor or record these emails

Green Cap
Green Cap
Green Cap
End Cap
More Sponsors
End Cap


Bohr's Atom and Spectral Lines

Bohr's model of the atom envisaged a nucleus around which electrons circulate in one or more distinct orbits (also called shells or energy bands or more recently orbitals). Each shell may carry one or more electrons or none at all. The shells and the electrons in them have characteristic quantised energy levels. The shell or orbit n1 closest to the nucleus is known as the ground state and has the lowest energy level. Orbits n2, n3 etc. progressively further away from the nucleus have correspondingly higher energy levels.

n is also known as the quantum number representing the energy state of the atom.

See more about Bohr's Model.

The Bohr Atom and Quantum Jumps

Quantum Jumps

  • Photon Emission
  • Heat or other stimuli may cause an electron to break out of its energy band and jump over one or more energy bands down to a lower energy orbit releasing a photon with a quantum of energy corresponding to the difference in energy level between the two orbits.

  • Photon Absorption
  • Conversely, when photons collide with an atom, their energy may be transferred to and absorbed by the atom's electrons causing them to jump to a higher energy level orbit.

The frequency f of the light energy released or absorbed in the quantum jump is given by Planck's Law E= hf where E is the difference in energy levels between the initial orbit and the final orbit and h is Planck's constant.

The corresponding wavelength λ is given by λ = c/f where c is the speed of light.


Spectral Lines

The dark lines in the Sun's radiation spectrum were first catalogued by Fraunhofer in 1814 and subsequently investigated by Kirchhoff and Bunsen who provided the initial analysis an explanation of atomic spectral lines.

The spectral lines of light emitted by an atom are known as its characteristic frequencies. They are the frequencies associated with the energy released or absorbed when an electron jumps from one discrete energy level to another.


In the hydrogen spectrum opposite, the spectral line with a wavelength of 656 nm (or frequency of 457,000 GHz) corresponds to an energy difference of 4.5 x 10-5 eV between the electron's ground state and its excited state, known as the fine structure enrgy gap.

Atomic Spectral Lines

White Light

White light consists of a continuous spectrum of frequencies resulting from so called black body radiation which encompasses radiation emitted from multiple different elements and the electron jumps between their multiple energy bands.


Atomic Emission Spectrum

This is the light generated by stimulating a source consisting of a sample of single element type. In the case of the hydrogen atoms, in the example above each individual atom in the sample has five potential quantised energy bands, only one of which is occupied by an electron at any time. The emission spectrum shown has 4 distinct bright spectral lines or colours with frequencies corresponding to quantum electron jumps from one of four excited states down to the ground state.


Atomic Absorption Spectrum

This describes the effect on a beam of white light passing through a cool (unstimulated) sample of vapour of a particular element. In the case of white light passing through a sample of hydrogen vapour with its electrons in the ground state, the energy of the photons in the light beam with frequencies corresponding the hydrogen's energy levels will be absorbed by the hydrogen atoms, causing their electrons to jump to higher quantised energy levels. The missing photons will leave corresponding gaps in the spectrum of the white light source which appear as four dark lines on the spectrum with exactly the same characteristic frequencies as in the emission spectrum.

Zeeman Effect Diagram of Zeeman Effect on Atomic Spectra

When an atom is placed in a strong static magnetic field its spectral lines are split into several components due to the distortion of the shape of the electron orbitals caused by the magnetic field which in turn changes the spacing of the energy levels of the atom. The effect was first observed by Zeeman in 1896 and is named after him.

The example opposite shows how the atomic absorption spectrum is affected by the application of the magnetic field. Known as the "nornal Zeeman effect", it was developed before the quantum effects had been discovered and corresponds to the properties of "zero spin" electrons. The application of quantum theory explained a similar splitting effect, known as the so called "anomalous Zeeman effect", which is due to the different quantised spins of the individual charged electrons giving them different magnetic moments which react with the applied magnetic field to produce a wider, finer spectrum of multiple sub-states of equal energy.

The distance between the Zeeman sub-levels is a function of magnetic field strength and this effect can be used to measure the magnetic field strength affecting radiation sources such as the Sun and the stars as well as laboratory plasmas.

Stark Effect

Analogous to the Zeeman effect, the Stark effect describes the splitting of the spectral lines caused electric fields.

Lamb Shift

This is the splitting of the 656 nm spectral line of the hydrogen atom, first observed by Lamb in 1947, due to the different orbital shapes of the ground state electrons. This creates a frequency difference of 1.057 GHz, known as the Lamb shift, between the two spectral lines which corresponds to a small energy gap of 4.372 x 10-6 eV between the excited states of its p and s ground state electrons. This is about 10% of the atom's fine structure energy gap. (See above)

This spread of the spectral lines is due to the interaction between the two different electron orbitals with the positive atomic nucleus and occurs in the absence of external magnetic or electric fields. It is thus not the same as the splitting due to the Zeeman and Stark effects which depend on the presence of such fields.



Using atomic spectroscopy, the characteristic emission and absorption spectra of individual elements provide unque fingerprints which can be used to identify their presence, not just in lab samples, but also in the radiation coming from remote stars and planets.






Printer image Print This Page || Home || FAQ || Site Map || Legal || Privacy Promise || Contacts


Woodbank Communications Ltd, South Crescent Road, Chester, CH4 7AU, (United Kingdom)
Copyright © Woodbank Communications Ltd 2005

End cap