Question: What is the name for the location where the solar wind collides with the interstellar wind?
About the article "Solar System", section "Heliopause".

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In astrophysics, a bow shock is the area between a magnetosphere and an ambient medium.
For stars, this boundary is typically the edge of the astrosphere, where the stellar wind meets the interstellar medium.
For a planetary magnetosphere, the bow shock is the boundary at which the speed of the stellar wind abruptly drops as a result of its approach to the magnetopause.
The best-studied example of a bow shock is that occurring where the Sun's wind encounters Earth's magnetopause, although bow shocks occur around all magnetized planets, such as Jupiter or Saturn.
Earth's bow shock is about thick and located about from the planet.
For several decades, the solar wind has been thought to form a bow shock at the edge of the heliosphere, where it collides with the surrounding interstellar medium.
This long-held belief was called into question in 2012 when data from the Interstellar Boundary Explorer (IBEX) found the Sun and heliosphere to be moving more slowly through the interstellar medium than previously believed.
This new finding suggests that beyond our Solar System's termination shock and heliopause, there may be no, or very little bow shock. 
The magnetopause is the abrupt boundary between a magnetosphere and the surrounding plasma.
For planetary science, the magnetopause is the boundary between the planet’s magnetic field and the solar wind.
The location of the magnetopause is determined by the balance between the pressure of the dynamic planetary magnetic field and the dynamic pressure of the solar wind.
As the solar wind pressure increases and decreases, the magnetopause moves inward and outward in response.
Waves (ripples and flapping motion) along the magnetopause move in the direction of the solar wind flow in response to small scale variations in the solar wind pressure and to Kelvin-Helmholtz instability.
The solar wind is supersonic and passes through a bow shock where the direction of flow is changed so that most of the solar wind plasma is deflected to either side of the magnetopause, much like water is deflected before the bow of a ship.
The zone of shocked solar wind plasma is the magnetosheath.
At Earth and all the other planets with intrinsic magnetic fields, some solar wind plasma succeeds in entering and becoming trapped within the magnetosphere.
At Earth, the solar wind plasma which enters the magnetosphere forms the plasma sheet.
The amount of solar wind plasma and energy which enters the magnetosphere is regulated by the orientation of the interplanetary magnetic field which is embedded in the solar wind.
The Sun and other stars with magnetic fields and stellar winds have a solar magnetopause or heliopause where the stellar environment is bounded by the interstellar environment. 
The heliosphere's outer structure is determined by the interactions between the solar wind and the winds of interstellar space.
The solar wind streams away from the Sun in all directions at speeds of several hundred km/s in the Earth's vicinity.
At some distance from the Sun, well beyond the orbit of Neptune, this supersonic wind must slow down to meet the gases in the interstellar medium.
This takes place in several stages:  The solar wind is traveling at supersonic speeds within the Solar System.
At the termination shock, a standing shock wave, the solar wind falls below the speed of sound and becomes subsonic.
It was previously held that, once subsonic, the solar wind might be affected by the ambient flow of the interstellar medium: Its pressures were theorized to cause the solar wind to form a nose on one side and comet-like heliotail behind.
The area called the heliosheath.
However, scientific results in 2009 showed that this model is incorrect.
As of 2011, it is thought to be filled with a magnetic bubble "foam".
The outer surface of the heliosheath, where the heliosphere meets the interstellar medium, is called the heliopause.
This is the edge of the entire heliosphere.
Scientific results in 2009 adjusted this model.
In theory, the heliopause causes turbulence in the interstellar medium as the sun orbits the Galactic Center.
Outside the heliopause, would be a turbulent region caused by the pressure of the advancing heliopause against the interstellar medium.
However, the velocity of Solar wind relative to the interstellar medium is probably too low for a bow shock.  
Solar Wind Ion Mass Spectrometer (SWIMS) and Solar Wind Ion Composition Spectrometer (SWICS): These two instruments are time-of-flight mass spectrometers, each tuned for a different set of measurements.
They analyze the chemical and isotopic composition of solar wind and interstellar matter. 
The solar wind "blows a bubble" in the interstellar medium (the rarefied hydrogen and helium gas that permeates the galaxy).
The point where the solar wind's strength is no longer great enough to push back the interstellar medium is known as the heliopause, and is often considered to be the outer border of the Solar System.
The distance to the heliopause is not precisely known, and probably varies widely depending on the current velocity of the solar wind and the local density of the interstellar medium, but it is known to lie far outside the orbit of Pluto.
Scientists hope to gain more perspective on the heliopause from data acquired through the Interstellar Boundary Explorer (IBEX) mission, launched in October 2008.