White Dwarf
What is white Dwarf?
A white dwarf is a comparatively small, dense type of star that is organized when a main determine star burns all of its hydrogen and helium fuel but lacks the force and heat necessity to fuse carbon and oxygen. The transformation of a star into a white dwarf begins when a main sequence star, around the mass of our Sun, burns up all its hydrogen fuel and starts being forced to fuse helium into carbon and oxygen. After billions of years, it is predicted that white dwarfs cool to become black dwarfs, lifeless stellar husks, although the age of the universe (13.7 billion years) has not been sufficient for this to occur yet.
When all the hydrogen in the star is mixed, feeling takes over and the star commences to fall in on itself. If the star is sufficiently heavy, a supernova may occur. Otherwise, the excess fabric just floats away to form a planetary nebula, and only the super-dense core remains, which is the white dwarf. The first white dwarf was observed by Friedrich Herschel on 31 January 1783, in a binary system, Eridani B and C.
Looking for anything Else ? Try Our Search
