Image description: The heliosphere protects the solar system from energetic cosmic rays; beyond this border lie the conditions of interstellar space, which is extremely thin compared to Earth's atmosphere. The heliopause marks the boundary where solar particle winds meet other particles from the interstellar medium. The diffuse interstellar medium is composed of matter that fills the space between stars. Interstellar matter is mainly composed of ionized hydrogen (H+), atomic hydrogen (H1), molecular hydrogen (H2), helium, grains a few tens to hundreds of nanometers in size, and much larger dust particles, a few micrometers in size.
The thermonuclear reactions that occur inside the Sun release enormous amounts of energy. Most of this energy is released into nearby space in the form of electromagnetic radiation, primarily visible light.
The Sun also emits a flux of charged particles called the Solar Wind. The solar wind is bimodal, a mixture of several types of winds, fast (3 million km/h) at high solar latitudes above 40°, and slow (1 million km/h) at latitudes between 22°S and 21°N. The solar wind is ionized, with electrons and protons separated, forming a plasma that travels to the far reaches of the solar system.
The Heliopause is the final frontier of the solar system, located at approximately 130 AU (20 billion km), where the solar wind fades and interstellar space begins.
At this point, the solar wind collides with opposing winds from the interstellar medium. Its push is no longer sufficient to repel the rarefied hydrogen and helium of the Galaxy.
The distance to the heliopause is not precisely known because it likely varies depending on the speed of the solar wind and the temporal density of the interstellar medium. In this region, known as the "magnetic highway," the instruments on the Voyager 1 probe recorded the highest rate of cosmic rays from interstellar space and a sharp decrease in particles from the Sun.
The Termination Shock is an intermediate boundary located before the heliopause. This region between the termination shock and the heliopause is called the Heliosheath.
The heliosheath is the turbulent zone where the solar wind is slowed and then compressed by interstellar pressure. When particles emitted by the Sun (a few particles per cubic centimeter) collide with interstellar particles, they slow down, heat up, and emit energy. These highly energized particles accumulate in front of the heliopause and create a shock wave. This shock wave is a trace left by the Sun during its journey through the Milky Way, which it traverses in approximately 220 million years.
N.B.: The three units of measurement in astronomy for expressing distances.
The Ecliptic or the Apparent Orbit of the Sun 
Solar maximum and minimum 
How to weigh
the sun? 
The spicules of the Blue Sun 
Explanation of the 8 of the analemma 
Superb annular eclipse of 2010 
The ring of fire from March 2010 
The
gigantic power of the Sun 
Our satellites also observe eclipses 
Simulator, the revolution of the planets around the Sun 
The
solar system ice line 
Tourist trip in the solar system 
Finally the return of sunspots in 2010 
Solar pillar, a link between sky and earth 
The infernal journey of the photon or random walk 
The most violent solar flares 
Baily grains in a solar eclipse 
2003 transit of Mercury in front of the Sun 
The Sun is a yellow dwarf star 
Grains of Baily or pearls of light 
Sunlight and wavelengths 
The chaotic formation of the solar system 
The perfect
solar storm 
Coronal mass ejections 
The Sun's angular momentum paradox 
Transit of the planet Venus on June 6, 2012 
Transit of the Moon in front of the Sun seen from space in 2007 
Solar Winds: A Key Phenomenon of Interplanetary Space 
Heliosphere: At the Borders of the Solar System
Chaos and sensitivity to initial conditions