Question: The magnetic pole is how far away from the "auroral zone"?
About the article "Aurora", section "Forms and magnetism".

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Typically the aurora appears either as a diffuse glow or as "curtains" that approximately extend in the east-west direction.
At some times, they form "quiet arcs"; at others ("active aurora"), they evolve and change constantly.
Each curtain consists of many parallel rays, each lined up with the local direction of the magnetic field lines, suggesting that auroras are shaped by Earth's magnetic field.
Indeed, satellites show that electrons are guided by magnetic field lines, spiraling around them while moving toward Earth.
The similarity to curtains is often enhanced by folds called "striations".
When the field line guiding a bright auroral patch leads to a point directly above the observer, the aurora may appear as a "corona" of diverging rays, an effect of perspective.
Although it was first mentioned by Ancient Greek explorer/geographer Pytheas, Hiorter and Celsius first described in 1741 evidence for magnetic control, namely, large magnetic fluctuations occurred whenever the aurora was observed overhead.
This indicates (it was later realized) that large electric currents were associated with the aurora, flowing in the region where auroral light originated.
Kristian Birkeland (1908) deduced that the currents flowed in the east-west directions along the auroral arc, and such currents, flowing from the dayside toward (approximately) midnight were later named "auroral electrojets" (see also Birkeland currents).
Still more evidence for a magnetic connection are the statistics of auroral observations.
Elias Loomis (1860) and later in more detail Hermann Fritz (1881) and S. Tromholt (1882) established that the aurora appeared mainly in the "auroral zone", a ring-shaped region with a radius of approximately 2500 km around Earth's magnetic pole.
It was hardly ever seen near the geographic pole, which is about 2000 km away from the magnetic pole.
The instantaneous distribution of auroras ("auroral oval") is slightly different, centered about 3–5 degrees nightward of the magnetic pole, so that auroral arcs reach furthest toward the equator about an hour before midnight.
The aurora can be seen best at this time, called magnetic midnight, which occurs when an observer, the magnetic pole in question and the Sun are in alignment.
In the 1970s, astrophysicist Joan Feynman deduced that auroras are a product of the interaction between the Earth's magnetosphere and the magnetic field of the solar wind.
Her work resulted from data collected by the Explorer 33 spacecraft.
On 26 February 2008, THEMIS probes were able to determine, for the first time, the triggering event for the onset of magnetospheric substorms.
Two of the five probes, positioned approximately one third the distance to the moon, measured events suggesting a magnetic reconnection event 96 seconds prior to auroral intensification.
Dr. Vassilis Angelopoulos of the University of California, Los Angeles, the principal investigator for the THEMIS mission, claimed, "Our data show clearly and for the first time that magnetic reconnection is the trigger."
Auroras are classified as diffuse and discrete.
The diffuse aurora is a featureless glow in the sky that may not be visible to the naked eye, even on a dark night.
It defines the extent of the auroral zone.
The discrete auroras are sharply defined features within the diffuse aurora that vary in brightness from just barely visible to the naked eye, to bright enough to read a newspaper by at night.
Discrete auroras are usually seen in only the night sky, because they are not as bright as the sunlit sky.
Auroras occasionally occur poleward of the auroral zone as diffuse patches or arcs, which are generally subvisual.
In northern latitudes, the effect is known as the aurora borealis (or the northern lights), named after the Roman goddess of dawn, Aurora, and the Greek name for the north wind, Boreas, by Pierre Gassendi in 1621.
Auroras seen near the magnetic pole may be high overhead, but from farther away, they illuminate the northern horizon as a greenish glow or sometimes a faint red, as if the Sun were rising from an unusual direction.
Discrete auroras often display magnetic field lines or curtain-like structures, and can change within seconds or glow unchanging for hours, most often in fluorescent green.
The aurora borealis most often occurs near the equinoxes.
The northern lights have had a number of names throughout history.
The Cree call this phenomenon the "Dance of the Spirits".
In Medieval Europe, the auroras were commonly believed to be a sign from God.
Its southern counterpart, the aurora australis (or the southern lights), has features that are almost identical to the aurora borealis and changes simultaneously with changes in the northern auroral zone.
It is visible from high southern latitudes in Antarctica, South America, New Zealand, and Australia.
Auroras occur on other planets.
Similar to the Earth's aurora, they are visible close to the planet's magnetic poles.
Modern style guides recommend that the names of meteorological phenomena, such as "aurora borealis", be uncapitalized. 
An aurora (plural: auroras or aurorae; from the Latin word "aurora", "sunrise" or the Roman goddess of dawn) is a natural light display in the sky particularly in the high latitude (Arctic and Antarctic) regions, caused by the collision of energetic charged particles with atoms in the high altitude atmosphere (thermosphere).
The charged particles originate in the magnetosphere and solar wind and, on Earth, are directed by the Earth's magnetic field into the atmosphere.
Most auroras occur in a band known as the "auroral zone", which is typically 3° to 6° wide in latitude and observed at 10° to 20° from the geomagnetic poles at all local times (or longitudes).
During a geomagnetic storm, the auroral zone expands to lower latitudes. 
Previous single and two-spacecraft missions were not capable of providing the data required to accurately study the boundaries of the magnetosphere.
Because the plasma comprising the magnetosphere cannot presently be accessed using remote sensing techniques, satellites must be used to measure it in-situ.
Four spacecraft allow scientists make the 3D, time-resolved measurements needed to create a realistic picture of the complex plasma interactions occurring between regions of the magnetosphere and between the magnetosphere and the solar wind.
Each satellite carries a scientific payload of 11 instruments designed to study the small-scale plasma structures in space and time in the key plasma regions: solar wind, bow shock, magnetopause, polar cusps, magnetotail, plasmapause boundary layer and over the polar caps and the auroral zones.
The bow shock is the region in space between the Earth and the sun where the solar wind decelerates from super- to sub-sonic before being deflected around the Earth.
In traversing this region, the spacecraft make measurements which help characterize processes occurring at the bow shock, such as the origin of hot flow anomalies and the transmission of electromagnetic waves through the bow shock and the magnetosheath from the solar wind.
Behind the bow shock is the thin plasma layer separating the Earth and solar wind magnetic fields known as the magnetopause.
This boundary moves continuously due to the constant variation in solar wind pressure.
Since the plasma and magnetic pressures within the solar wind and the magnetosphere, respectively, should be in equilibrium, the magnetosphere should be an impenetrable boundary.
However, plasma has been observed crossing the magnetopause into the magnetosphere from the solar wind.
Cluster's four-point measurements make it possible to track the motion of the magnetopause as well as elucidate the mechanism for plasma penetration from the solar wind.
In two regions, one in the northern hemisphere and the other in the south, the magnetic field of the Earth is perpendicular rather than tangential to the magnetopause.
These polar cusps allow solar wind particles, consisting of ions and electrons, to flow into the magnetosphere.
Cluster records the particle distributions, which allow the turbulent regions at the exterior cusps to be characterized.
The regions of the Earth's magnetic field that are stretched by the solar wind away from the sun are known collectively as the magnetotail.
Two lobes that reach past the Moon in length form the outer magnetotail while the central plasma sheet forms the inner magnetotail, which is highly active.
Cluster monitors particles from the ionosphere and the solar wind as they pass through the magnetotail lobes.
In the central plasma sheet, Cluster determines the origins of ion beams and disruptions to the magnetic field-aligned currents caused by substorms.
The precipitation of charged particles in the atmosphere creates a ring of light emission around the magnetic pole known as the auroral zone.
Cluster measures the time variations of transient particle flows in the region.  
Any system possessing a net magnetic dipole moment m will produce a dipolar magnetic field (described below) in the space surrounding the system.
While the net magnetic field produced by the system can also have higher-order multipole components, those will drop off with distance more rapidly, so that only the dipolar component will dominate the magnetic field of the system at distances far away from it.
The vector potential of magnetic field produced by magnetic moment m is  formula_15 and magnetic flux density is  formula_16 Alternatively one can obtain the scalar potential first from the magnetic pole perspective, formula_17 and hence magnetic field strength is formula_18 The magnetic field of an ideal magnetic dipole is depicted on the left.