Heliopause
What is the meeting point of solar and interstellard wind called?
Solar System
Coronal mass ejection Interplanetary scintillation Magnetosphere of Saturn Index of solar energy articles Electric sail
Coronal_mass_ejection-NASA_mission_"Wind" Interplanetary_scintillation-Solar_wind Magnetosphere_of_Saturn-Size_and_shape Index_of_solar_energy_articles-S Electric_sail-Abstract
Related solar observation missions.NASA mission "Wind". On 1 November 1994, NASA launched the WIND spacecraft as a solar wind monitor to orbit Earth's Lagrange point as the interplanetary component of the Global Geospace Science (GGS) Program within the International Solar Terrestrial Physics (ISTP) program. The spacecraft is a spin axis-stabilized satellite that carries eight instruments measuring solar wind particles from thermal to >MeV energies, electromagnetic radiation from DC to 13 MHz radio waves, and gamma-rays. Though the WIND spacecraft is nearly two decades old, it still provides the highest time, angular, and energy resolution of any of the solar wind monitors. It continues to produce relevant research as its data has contributed to over 150 publications since 2008 alone. 
Solar wind. As interplanetary scintillation is caused by the solar wind, measurements of interplanetary scintillation "be utilized as valuable and inexpensive probes of the solar wind." As already noted, the observed information, the intensity fluctuations, is related to the desired information, the structure of the solar wind, through the phase change experienced by waves traveling through the solar wind. The root mean square (RMS) intensity fluctuations are often expressed relative to the mean intensity from the source, in a term called the scintillation index, which is written asformula_1This can be related to the phase deviation caused by turbulence in the solar wind by considering the incident electromagnetic plane wave, and yieldsformula_2The next step, relating the phase change to the density structure of the solar wind, can be made more simple by assuming that the density of the plasma is highest towards the sun, which allows the "thin screen approximation." Doing so eventually gives an RMS deviation for the phase offormula_3where formula_4 is the wavelength of the incoming wave, formula_5 is the classical electron radius, formula_6 is the thickness of the "screen," or the length scale over which the majority of the scattering takes place, formula_7 is the typical size scale of density irregularities, and formula_8 is the root mean squared variation of the electron density about the mean density. Thus interplanetary scintillation can be used as a probe of the density of the solar wind. Interplanetary scintilation measurements may also be used to infer the velocity of the solar wind. Stable features of the solar wind can be particularly well studied. At a given time, observers on Earth have a fixed line of sight through the solar wind, but as the Sun rotates over an approximately month long period, the perspective on Earth changes. It is then possible to do "tomographic reconstruction of the distribution of the solar wind" for the features of the solar wind which remain static. 
Saturn's internal magnetic field deflects the solar wind, a stream of ionized particles emitted by the Sun, away from its surface, preventing it from interacting directly with its atmosphere and instead creating its own region, called a magnetosphere, composed of a plasma very different from that of the solar wind. The magnetosphere of Saturn is the second–largest magnetosphere in the Solar System after that of Jupiter. As with Earth's magnetosphere, the boundary separating the solar wind's plasma from that within Saturn's magnetosphere is called the magnetopause. The magnetopause distance from the planet's center at the subsolar point varies widely from 16 to 27 Rs (Rs=60,330 km is the equatorial radius of Saturn). The magnetopause's position depends on the pressure exerted by the solar wind, which in turn depends on solar activity. The average magetopause standoff distance is about 22 Rs. In front of the magnetopause (at the distance of about 27 Rs from the planet) lies the bow shock, a wake-like disturbance in the solar wind caused by its collision with the magnetosphere. The region between the bow shock and magnetopause is called the magnetosheath. At the opposite side of the planet, the solar wind stretches Saturn's magnetic field lines into a long, trailing magnetotail, which consists of two lobes, with the magnetic field in the northern lobe pointing away from Saturn and the southern pointing towards it. The lobes are separated by a thin layer of plasma called the tail current sheet. Like Earth’s, Saturn's tail is a channel through which solar plasma enters the inner regions of the magnetosphere. Similar to Jupiter, the tail is the conduit through which the plasma of the internal magnitospheric origin leaves the magnetosphere. The plasma moving from the tail to the inner magnitopshere is heated and forms a number of radiation belts. 
An Electric sail (also called electric solar wind sail or E-Sail) is a proposed form of spacecraft propulsion using the dynamic pressure of the solar wind as a source of thrust. It uses an electric field for deflecting solar wind protons and extracting momentum from them. It was invented by Pekka Janhunen from Finland in 2006 at the FMI and creates a "virtual" sail by forming an electric field on small wires.  