When the solar wind is strong enough, the top part of the aurora appears. It is often red: https://commons.wikimedia.org/w/index.php?title=File%3AAurora_Australis.ogv.

The aurora is the product of the following steps:

  1. A charged particle from solar wind follows one of Earth's magnetic field lines downwards and polewards.
  2. The charged particle collides with a atmospheric particle. An electron in the atmospheric particle is excited to a higher energy level.
  3. After some delay, the electron relaxes to a lower energy level, either a) by emitting light, or b) during a collision with another atmospheric particle.

The two most common aurora colours, green and red are emitted by atomic [non-molecular] oxygen (wavelengths 558 and 630 nm, respectively). Importantly, the decay which emits green light occurs more rapidly than the red one.

At medium altitudes, atomic oxygen is quite abundant. Atom-atom collisions (step 3b) are quite common, so the slow emission of red light is suppressed. The aurora appears green.

At higher altitudes, atomic oxygen is rare. Atom-atom collisions are rare, so red light can also be emitted. This is the standard explanation for why the top of the aurora is red.

However, this explanation does not seem complete. There is no reason why green light should not be emitted at high altitudes (in addition to red light). So why is the top of the aurora red (with no trace of green)?

  • $\begingroup$ Or simply above you have a more reddish light. Might be there is another reason (nitrogen? ) but we tend to forget that our vision is tailored to give us a feeling of bright and white for the solar spectrum as filtered by atmosphere. All the rest is a fine balance. $\endgroup$
    – Alchimista
    Commented Jan 17, 2018 at 10:24
  • $\begingroup$ I guess that the reason is the spectrum of atomic O at low density has a more intense emission peak at 630 nm than at 558 nm, but I can't find a plot of it. $\endgroup$
    – valerio
    Commented Jan 26, 2018 at 12:08

2 Answers 2


It's because there's more nitrogen at lower heights:

The green color of the aurora below 150 km height stems from the 558 nm line of Oxygen. It is not seen at larger heights since the 1S-state is not reached from the 3P ground state in collisions with electrons or protons. It is assumed that this state is produced in collisions of O(3P) with excited nitrogen molecules which give off their energy and take over angular momentum: $N_2^* + O(^3P) → N_2 + O(^1S)$

By Dietrich Zawischa's Atomic spectra webpage.

Oxygen becomes more common than nitrogen at heights above ~150 km (see figure below), where the help from nitrogen then becomes less likely to take place:




The aurora are caused by energetic electrons and protons impacting the atmosphere and exciting the atoms which then re-emit light. I have more background info in the following answer: https://physics.stackexchange.com/a/335325/59023 .

The red light is from atomic oxygen and is at a ~630.0 nm wavelength. The dominant green light is from diatomic nitrogen at a ~557.7 nm wavelength (see image below). This much you seem to already know.

There is no reason why green light should not be emitted at high altitudes (in addition to red light). So why is the top of the aurora red (with no trace of green)?

Diatomic nitrogen is much heavier than monatomic oxygen, i.e., ~28 amu vs. ~16. Thus, if the gas is in thermal equilibrium – all constituents share the same temperature but heat fluxes can exist – then the monatomic oxygen will have a higher thermal speed than the N2. Thus, the oxygen atoms can migrate to higher altitudes more easily than the N2 molecules1.

Courtesy of NCAR/HAO: Aurora Emission Spectrum

Further, monatomic oxygen is more easily ionized than monatomic nitrogen with ionization energies of ~1313.9 kJ mol-1 and ~1402.3 kJ mol-1 (or ~13.62 eV and ~14.53 eV), respectively (there is a full list at https://en.wikipedia.org/wiki/Ionization_energies_of_the_elements_(data_page)). That is assuming that the diatomic nitrogen dissociated into two monatomic nitrogen atoms.

Dissociation of N2 requires ~945 kJ mol-1 or ~9.79 eV, or a photon with a frequency of ~2.368 x 1015 Hz = 2368 THz or ~126.6 nm. This is in the far to extreme ultraviolet radiation range2. $\color{blue}{\textbf{The problem is that $N_{2}$ is mostly transparent to wavelengths near 100 nm.}}$ Further, the shorter wavelengths that are absorbed by N2 do not make it deep enough into the atmosphere.

So why is the top of the aurora red (with no trace of green)?

Be careful here because the bottom of the aurora has red-to-magenta-to-violet colors as well, but much more faint. So we often do not see them with our eyes unless it's a very strong geomagnetic storm, in which case most of the emission is red, not green3.


  1. The separation starts to occur above ~85 km in altitude.
  2. This is also in the UVC range, which can penetrate down to ~40-50 km and has the highest interaction cross-section with diatomic and triatomic oxygen (i.e., ozone).
  3. The emissions are also seen at much lower latitudes than normal, sometimes down to the Caribbean as in the Carrington event of 1859.

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