Question: What are typical values for speed, density and intensity for the solar wind?
About the article "Aurora", section "Solar wind and the magnetosphere".

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Solar wind.
As interplanetary scintillation is caused by the solar wind, measurements of interplanetary scintillation "be utilized as valuable and inexpensive probes of the solar wind."
As already noted, the observed information, the intensity fluctuations, is related to the desired information, the structure of the solar wind, through the phase change experienced by waves traveling through the solar wind.
The root mean square (RMS) intensity fluctuations are often expressed relative to the mean intensity from the source, in a term called the scintillation index, which is written asformula_1This can be related to the phase deviation caused by turbulence in the solar wind by considering the incident electromagnetic plane wave, and yieldsformula_2The next step, relating the phase change to the density structure of the solar wind, can be made more simple by assuming that the density of the plasma is highest towards the sun, which allows the "thin screen approximation."
Doing so eventually gives an RMS deviation for the phase offormula_3where formula_4 is the wavelength of the incoming wave, formula_5 is the classical electron radius, formula_6 is the thickness of the "screen," or the length scale over which the majority of the scattering takes place, formula_7 is the typical size scale of density irregularities, and formula_8 is the root mean squared variation of the electron density about the mean density.
Thus interplanetary scintillation can be used as a probe of the density of the solar wind.
Interplanetary scintilation measurements may also be used to infer the velocity of the solar wind.
Stable features of the solar wind can be particularly well studied.
At a given time, observers on Earth have a fixed line of sight through the solar wind, but as the Sun rotates over an approximately month long period, the perspective on Earth changes.
It is then possible to do "tomographic reconstruction of the distribution of the solar wind" for the features of the solar wind which remain static. 
The Earth is constantly immersed in the solar wind, a rarefied flow of hot plasma (gas of free electrons and positive ions) emitted by the Sun in all directions, a result of the million-degree heat of the Sun's outermost layer, the solar corona.
The solar wind usually reaches Earth with a velocity around 400 km/s, density around 5 ions/cc and magnetic field intensity around 2–5 nT (nanoteslas; Earth's surface field is typically 30,000–50,000 nT).
These are typical values.
During magnetic storms, in particular, flows can be several times faster; the interplanetary magnetic field (IMF) may also be much stronger.
The IMF originates on the Sun, related to the field of sunspots, and its field lines (lines of force) are dragged out by the solar wind.
That alone would tend to line them up in the Sun-Earth direction, but the rotation of the Sun skews them (at Earth) by about 45 degrees, so that field lines passing Earth may actually start near the western edge ("limb") of the visible sun.
When the solar wind is perturbed, it easily transfers energy and material into the magnetosphere.
The electrons and ions in the magnetosphere that are thus energized move along the magnetic field lines to the polar regions of the atmosphere. 
The Earth is constantly immersed in the solar wind, a rarefied flow of hot plasma (gas of free electrons and positive ions) emitted by the Sun in all directions, a result of the two-million-degree heat of the Sun's outermost layer, the corona.
The solar wind usually reaches Earth with a velocity around 400 km/s, density around 5 ions/cm3 and magnetic field intensity around 2–5 nT (nanoteslas; Earth's surface field is typically 30,000–50,000 nT).
These are typical values.
During magnetic storms, in particular, flows can be several times faster; the interplanetary magnetic field (IMF) may also be much stronger.
The IMF originates on the Sun, related to the field of sunspots, and its field lines (lines of force) are dragged out by the solar wind.
That alone would tend to line them up in the Sun-Earth direction, but the rotation of the Sun skews them (at Earth) by about 45 degrees, so that field lines passing Earth may actually start near the western edge ("limb") of the visible Sun.
Earth's magnetosphere is formed by the impact of the solar wind on the Earth's magnetic field.
It forms an obstacle to the solar wind, diverting it, at an average distance of about 70,000 km (11 Earth radii or Re), forming a bow shock 12,000 km to 15,000 km (1.9 to 2.4 Re) further upstream.
The width of the magnetosphere abreast of Earth, is typically 190,000 km (30 Re), and on the night side a long "magnetotail" of stretched field lines extends to great distances (> 200 Re).
The magnetosphere is full of trapped plasma as the solar wind passes the Earth.
The flow of plasma into the magnetosphere increases with increases in solar wind density and speed, with increase in the southward component of the IMF and with increases in turbulence in the solar wind flow.
The flow pattern of magnetospheric plasma is from the magnetotail toward the Earth, around the Earth and back into the solar wind through the magnetopause on the day-side.
In addition to moving perpendicular to the Earth's magnetic field, some magnetospheric plasma travel down along the Earth's magnetic field lines and lose energy to the atmosphere in the auroral zones.
Magnetospheric electrons accelerated downward by field-aligned electric fields cause the bright aurora features.
The un-accelerated electrons and ions cause the dim glow of the diffuse aurora.
  The intensity of electromagnetic radiation can be expressed in W/m2.
An example of such a quantity is the solar constant.
Wind turbines are often compared using a specific power measuring watts per square meter of turbine disk area, which is formula_1, where "r" is the length of a blade.
This measure is also commonly used for solar panels, at least for typical applications.
Radiance is surface power density per unit of solid angle (steradians) in a specific direction.
Spectral radiance is radiance per unit of frequency (Hertz) at a specific frequency.  
The solar wind is divided into two components, respectively termed the slow solar wind and the fast solar wind.
The slow solar wind has a velocity of about 400 km/s, a temperature of 1.4–1.6 K and a composition that is a close match to the corona.
By contrast, the fast solar wind has a typical velocity of 750 km/s, a temperature of 8 K and it nearly matches the composition of the Sun's photosphere.
The slow solar wind is twice as dense and more variable in intensity than the fast solar wind.
The slow wind also has a more complex structure, with turbulent regions and large-scale structures.
The slow solar wind appears to originate from a region around the Sun's equatorial belt that is known as the "streamer belt".
Coronal streamers extend outward from this region, carrying plasma from the interior along closed magnetic loops.
Observations of the Sun between 1996 and 2001 showed that emission of the slow solar wind occurred between latitudes of 30–35° around the equator during the solar minimum (the period of lowest solar activity), then expanded toward the poles as the minimum waned.
By the time of the solar maximum, the poles were also emitting a slow solar wind.
The fast solar wind is thought to originate from coronal holes, which are funnel-like regions of open field lines in the Sun's magnetic field.
Such open lines are particularly prevalent around the Sun's magnetic poles.
The plasma source is small magnetic fields created by convection cells in the solar atmosphere.
These fields confine the plasma and transport it into the narrow necks of the coronal funnels, which are located only 20,000 kilometers above the photosphere.
The plasma is released into the funnel when these magnetic field lines reconnect.