a. For calculation of engineering effects due to the solar wind, a flowing Maxwellian distribution shall be used, with density and temperature given in Table 8‑2.
b. Spacecraft in L1 and L2 shall be considered to experience the same mean and range of plasma parameters in the solar wind as at the Earth.
NOTE Because the solar wind flows through the near-Earth interplanetary medium with negligible modification (unless it encounters the bow shock), the mean and range of plasma density and temperature can be considered spatially uniform in the vicinity of 1AU. However, variations in plasma at the Earth are seen at L1 and L2 between approximately 30 and 90 minutes earlier or later, respectively.
c. A r-2 variation shall be used to map the mean and range of solar wind density to other locations in the heliosphere in the ecliptic plane, where r is heliocentric distance.
d. A r-0,64 variation shall be used to map the mean and range of the electron temperature to other locations in the heliosphere in the ecliptic plane.
e. The ion temperature and composition shall be assumed to be the same as near the Earth.