This module allows you to experiment with a phenomenological model of stream interactions based on a parameterized treatment of the physics (described by Hakamada, K., and S.-I. Akasofu, Simulation of Three-Dimensional Solar Wind Disturbances and Resulting Geomagnetic Storms, Space Sci. Rev., 31, 3-70, 1982), and to “simulate” plasma and field data that might be observed by spacecraft at various heliocentric distances.
Spacecraft measurements show that the solar wind velocity depends on the distance from the heliospheric current sheet. The velocity can be 2 to 3 times as high near the magnetic “poles” of the Sun (the location of polar coronal holes) as it is near the current sheet. This “heliomagnetic latitude” dependence produces a high speed/low speed “stream” structure that is especially prominent at low heliographic latitudes when the dipole tilt is significant or a strong quadrupole contribution to the Sun’s field is present.
When there is a non-zero dipole tilt or finite quadrupole moment the solar rotation brings different source velocities to the base of a given radial direction in the inertial frame. Since the plasma transport is radial, high speed plasma that is launched behind lower speed plasma will plow into it and create a “stream interaction” region. Due to the fact that the magnetized plasmas do not interpenetrate, the interaction speeds up the slower plasma and slows down the faster plasma. A pressure ridge is thus formed that takes a spiral form for the same reasons as the interplanetary magnetic field (IMF).
The distribution of IMF magnitude also shows the interaction regions since it too is compressed. Collisionless shocks may eventually form as the pressure ridges steepen with increasing heliospheric distance, but this usually happens beyond 1 AU.
The graphs on the left show, from top to bottom:
The graphs on the right show the predicted 1 AU data versus time in steady state as the Sun rotates every 27 days, from top to bottom:
The controls on the left allow you to adjust the maximum velocity of the observer (out to 1 AU), the quadrupole to dipole ratio, and the tilt angle of the dipole moment. This later angle is set to zero if the quadrupole moment is non-zero. The slow region around the neutral sheet (magnetic equator) has a fixed Gaussian width and variable depth.
Note: For additional information, click Help in the Solar Wind: Neutral Sheet Model, 3-D Structure module.