What is a white dwarf?

The white dwarf is a relatively small, dense type of star that is formed when the main sequential star burns all hydrogen and helium fuel, but lacks the pressure and heat necessary for the carbon and oxygen fuse. The white dwarf usually has a weight between 0.5 and 0.7 times the sun, but a volume comparable to the ground volume. The white dwarf is the final state of stellar development for 97% of known stars. Since its core begins to build with carbon and oxygen that cannot be connected, there must be a fusion on the shell outside the core. Huge core gravity pushes hydrogen together and causes it to join much faster than before, increasing the brightness of Star by a factor of 1,000 - 10,000 and increasing its radius to something comparable to Mars' orbit.

When all the hydrogen is fused in the star, gravity takes over, and the star starts to fall on herself. If the star is massive enough, supernova can occur. Otherwise the excess material hoves PRyt and creates a planetary nebula and remains only a super dense core, a white dwarf. Because the white dwarf does not have its own energy source, the only heat it produces is the rest of its helium. It has been assumed that white dwarfs will become cool dwarves, inanimate star peels, although the age of the universe (13.7 billion years) has not yet been enough.

white dwarves make up 6% of all stars in our sun district. Because there are no nuclear reactions in their core, they are not very clear, even if they are observable in strong telescopes. Sirius B, a companion of his more famous Hopartner, Sirius A, also known as Dog Star, is a white dwarf. The first white dwarf was watched by Friedrich Herschel on 31 January 1783 in the binary system Eridani B and C.