What is heliopause?
Heliopause is a boundary in a space where the outer pressure of our own sun wind, composed of gases and particles "blown" out by the forces generated by the sun oven, is equilibrium with internal pressure interstellar particles pushing on the heliosphere. The heliosphere is an area around the Sun, which is influenced by the sun magnetic field and in which the solar wind develops a recognizable pressure of the external pressure from the sun. Analogy would be a balloon with the sun inside. The solar wind is the air inflating balloon, the outer air is the pressure of the interstellar medium (ISM) and the balloon itself is a heliopause.
The existence of this boundary is accepted as a reality of modern science. What is still undetermined is its exact position and how it affects the interaction between the heliosphere and interstellar medium, which is interstellar space between solar systems. Astronomers and physicists have been induced by a lot of accurate positions and profile of the heliosphere and in the expansion of Heliopaus, but the exact data is not yet available. We hope that when a person boilBil probe, such as Voyager 1 and 2 and Pioneer 10, continue outwards on their way from the solar system to interstellar space, that more accurate information will be available.
Science is also generally accepted that the heliosphere is not a perfect sphere. This is because the sun moves through the interstellar space, and, as with the running river, the "upstream" of the heliosphere in the direction of solar travel is compressed, while the "downstream" side is prolonged. Astronomers estimate that the heliopause will be located approximately 100 to 150 astronomical units (AU) from the Sun in the direction of "upstream". The astronomical unit is an average distance from Earth to the sun or about 93 million miles (149 million kilometers). It is not known to the border of "downstream", but is considered somewhat further, perhaps in the range of 170 AU.
As a border, heliopause is not absolute. The particles from the outside of the heliosphere penetrate in and believe thatwhich particles of the solar wind pass through the border. It is assumed that there are two areas of compression and turbulence to the "upstream", where the magnetic fields form "bubbles". The solar wind, as it approaches for heliopause, reaches an area known as an end shock where it slows down significantly. In addition to Heliopauz, when the incoming flow of interstellar medium is close to the border, it also slows down the area known as the bow.