Many chemical reactions take place in the upper atmosphere to maintain
the ionosphere - a balance between the production of free electrons and their removal. There are also intermediate reactions that change the composition of the atmosphere above the homopause (about 100 km altitude). In the generic reactions below, upper case letters represent a molecule, γ represents a photon of electromagnetic energy (light, UV, EUV or X-ray), and e- is an electron.
X + γ → X+ + e- X- + Y → XY + e- |
photoionisation associative detachment |
XY + γ → X + Y X+ + YZ → YX+ + Z |
photodissociation charge exchange |
X+ + e- → X X+ + e- → X + γ YX+ + e- → Y + X X + e- → X- |
simple recombination radiative recombination dissociative recombination electron attachment |
The species that provide most of the ions in the ionosphere are oxygen (in both the diatomic and monatomic forms) and nitric oxide (specifically in the lower ionosphere).
The last two of these species are produced by the following reactions:
O2 + γ → O + O N + O2 → NO + O NO + N → N2 + O |
photodissociation production of nitric oxide removal of nitric oxide |
N2 + γ → N2 + e- N2+ + e- → N + N O+ + N2 → NO+ + N O + N2+ → NO+ + N |
photoionisation dissociative recombination charge exchange charge exchange |
H+ + O ↔ H + O+ | charge exchange |
O2 + e- + A → O2- + A | electron attachment (with catalyst) |
O2- + O → O3 + e- | associative detachment |
The above reactions form part of the photochemistry that churns daily above our heads as the solar electromagnetic influx varies in its diurnal cycle. In bulk they give rise to the changing ionosphere that makes possible long distance radio propagation but that is also the bane of radio astronomy and satellite navigation and communication.
Australian Space Academy