Question: How are the auroras made?
About the article "Aurora", section "Auroral mechanism".

Candidate passages:
Auroras occur on Mars, but they do not occur at the poles as on Earth, because Mars has no planetwide magnetic field.
Rather, they occur near magnetic anomalies in Mars's crust, which are remnants from earlier days when Mars did have a magnetic field.
Martian auroras are a distinct kind not seen elsewhere in the solar system.
They would probably also be invisible to the human eye, being largely ultraviolet phenomena. 
 "Walls Is Auroras" at Nippon Budokan  
The rayleigh is a unit of photon flux, used to measure airglow (auroras, for example).
It was first proposed in 1956 by D. M. Hunten, Franklin E. Roach, and J. W. Chamberlain.
It is named for Robert John Strutt, 4th Baron Rayleigh (1875–1947).
Its symbol is R (also used for the röntgen, an unrelated unit).
SI prefixes are used with the rayleigh.
One rayleigh (1 R) is defined as a column emission rate of 1010 photons per square metre per column per second.
Note that rayleigh is an apparent emission rate, as no allowances have been made for scattering or absorption.
The night sky has an intensity of about 250 R, while auroras can reach values of 1000 kR.
The relationship between photon radiance, "L", (in units of photons per square metre per second per steradian) and "I" (in units of rayleighs) is simply  formula_1  
AuroraMAX is a project which monitors and presents images of auroras seen from Yellowknife (Northwest Territories, Canada).
This project allows to amateur astronomers to watch auroras up to and during the solar maximum in 2013.
AuroraMAX is available only in French and in English.
Auroras are natural exhibition of lights that can be seen by the naked eyes.
Auroras happen when protons and electrons or charged particles and gases in the Earth's atmosphere crash into each other, creating tiny flares of light that decorate the sky with colorful light.
Billions of these tiny flares occur in sequence causing the lights to seem like they are dancing or moving.
The lights in the Northern hemisphere are Aurora Borealis or simply The Northern Lights while the lights in the Southern hemisphere are called Aurora Australis or simply The Southern Lights.
Amateur astronomers can see auroras online and live, through the AuroraMAX Online Observatory.
The project is a collaboration between the University of Calgary, the Canadian Space Agency, the society Astronomy North, and the city of Yellowknife. 
Intense columns of Auroral ionization at 100 km altitudes within the auroral oval backscatter radio waves, perhaps most notably on HF and VHF.
Backscatter is angle-sensitive—incident ray vs. magnetic field line of the column must be very close to right-angle.
Random motions of electrons spiraling around the field lines create a Doppler-spread that broadens the spectra of the emission to more or less noise-like—depending on how high radio frequency is used.
The radio-auroras are observed mostly at high latitudes and rarely extend down to middle latitudes.
The occurrence of radio-auroras depends on solar activity (flares, coronal holes, CMEs) and annually the events are more numerous during solar cycle maxima.
Radio aurora includes the so-called afternoon radio aurora which produces stronger but more distorted signals and after the Harang-minima, the late-night radio aurora (sub-storming phase) returns with variable signal strength and lesser doppler spread.
The propagation range for this predominantly back-scatter mode extends up to about 2000 km in east-west plane, but strongest signals are observed most frequently from the north at nearby sites on same latitudes.
Rarely, a strong radio-aurora is followed by Auroral-E, which resembles both propagation types in some ways.