Termination shock
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Image:Voyager 1 entering heliosheath region.jpg
In space physics, the termination shock is the boundary marking one of the outer limits of the sun's influence. It is where the bubble of solar wind particles slows down to subsonic speed (with respect to the star) due to interactions with the local interstellar medium. This causes compression, heating, and a change in the magnetic field. The termination shock is believed to be 75-90 astronomical units[1] from the Sun. The termination shock boundary fluctuates in its distance from the sun as a result of fluctuations in solar flare activity, i.e. changes in the ejections of gas and dust from the sun.
The shock arises because solar wind particles are emitted from stars at about 400 km/s, while the speed of sound is about 50 km/s. (The exact speed depends on the density, which fluctuates considerably.) The interstellar medium, although very low in density, nonetheless has a constant pressure associated with it; the pressure from the solar wind decreases with the square of the distance from the star. As one moves far enough away from the star, the pressure from the interstellar medium becomes sufficient to slow the solar wind down to below its speed of sound; this causes a shock wave.
Going outward from the sun, the termination shock is followed by the Heliopause where solar wind particles are stopped by the interstellar medium, then the Bow Shock past which particles from the interstellar medium are no longer excited.
Evidence presented at a meeting of the American Geophysical Union in May 2005 by Dr. Ed Stone suggests that the Voyager 1 spacecraft passed termination shock in December 2004 by virtue of the change in magnetic readings taken from the craft.