Question: Are these values typical?  400 km/s)
About the article "Aurora", section "Solar wind and the magnetosphere".

Candidate passages:
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 velocity of P-waves in a homogeneous isotropic medium is given by formula_1 where "K" is the bulk modulus (the modulus of incompressibility), "formula_2" is the shear modulus (modulus of rigidity, sometimes denoted as "G" and also called the second Lamé parameter), "formula_3" is the density of the material through which the wave propagates, and "formula_4" is the first Lamé parameter.
Of these, density shows the least variation, so the velocity is mostly "controlled" by "K" and "μ".
The elastic moduli P-wave modulus, formula_5, is defined so that formula_6 and thereby formula_7 Typical values for P-wave velocity in earthquakes are in the range 5 to 8 km/s.
The precise speed varies according to the region of the Earth's interior, from less than 6 km/s in the Earth's crust to 13 km/s through the core. 
Zeta Puppis (Zeta Pup, ζ Puppis, ζ Pup) is a star in the constellation of Puppis.
It is also known by the traditional names Naos (, from the Greek "ναύς" "ship") and Suhail Hadar (سهيل هدار, possibly "roaring bright one") in Arabic.
Its spectral class is O4If, making it an exceptionally hot star, and it is one of the sky's few naked-eye class O-type stars as well as the closest to Earth.
It had been assumed to be part of the Vela complex near the Gum nebula over 400 parsecs from Earth, but the 2008 reduction of Hipparcos data gave a distance of ± 4%.
Its surface temperature is 42,000 K .
The current mass is calculated at 22.5 solar masses and the radius at 14 times the solar radius but these values are highly uncertain.
Older derivations assumed the larger distance and were correspondingly larger, but some new calculations still give values up to twice these.
Zeta Puppis is an extreme blue supergiant, one of the most luminous stars in the Milky Way.
Visually, it is 12,500 times more powerful than the Sun, but being an extreme blue star, most of its radiation is in the ultraviolet and hence its bolometric luminosity is over 500,000 times that of the sun.
It is also the 62nd brightest star in terms of apparent magnitude from EarthZeta Puppis, being typical of O-type stars, is also notable for its extremely strong stellar wind, and it has garnered increasing attention for this over the past decade.
Its stellar wind velocity has been estimated at 2,500 km/s, which sees the star shed more than a millionth of its mass each year, or about 10 million times that shed by our own Sun over a comparable time period.
This mass ejection is highly evident in non-visible wavelengths such as radio and X-ray. 
Mike Brown considers the following bodies, ranked by estimated size, to be "probably" plutoids.
Asteroids are not considered.
The terms for varying degrees of likelihood are: Near certainty: Sufficient confidence to say these must be in hydrostatic equilibrium even if predominantly rocky.
Highly likely: Estimated/measured to be over 600 km.
The size would have to be "grossly in error" or they would have to be primarily rocky to not be dwarf planets.
Likely: Estimated/measured to be over 500 km.
Uncertainties in measurement mean that some of these will be significantly smaller and thus doubtful.
Probable: Estimated/measured to be over 400 km.
Expected to be dwarf planets if they are icy and that figure is correct.
All sizes are estimates.
Occultation probably gives the most exact estimate.
In cases without measurement, the "typical" albedo for an object is assumed from its absolute magnitude, and the size estimate is computed using these values.
Another 262 objects were listed as "possible" dwarfs, depending on composition and the accuracy of size and mass estimates. 
Randonneuring events must be undertaken within set time limits.
There is some regional variation in these, but the following list is typical: 200 km - 13.5 hours (14 hours in the UK, as in the original events.)
300 km - 20 hours 400 km - 27 hours 600 km - 40 hours 1000 km - 75 hours 1200 km - 90 hours (or 80 or 84 hours by choice) 1400 km - 116:40 hours (optionally 105:16 or 93:20 hours) Organisers are usually free to reduce the maximum speed.
(This sometimes makes it easier to man controls at particularly hilly events.)