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Hot Stars

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But not all white dwarfs cool the same way. Last year, astronomers found a certain type of massive white dwarf stars cool more slowly than others , as though they have an additional source of heat.

But figuring out what that heat source could be is proving tricky. We know now, thanks to new research, one thing that it isn't: the sedimentation, or inward sinking, of a neutron-rich stable isotope of neon deep in the stars' interiors.

Most stars in the Milky Way galaxy - those below about eight times the mass of the Sun - are destined to become white dwarf stars.

Stars of this mass, having run out of hydrogen and helium to fuse, have insufficient pressure to ignite the carbon that remains. They eject their outer material, and the core contracts into a sphere about the size of the Earth.

Stars spend 90 percent of their lives in their main sequence phase. Now around 4. As stars move toward the ends of their lives, much of their hydrogen has been converted to helium.

Helium sinks to the star's core and raises the star's temperature—causing its outer shell of hot gases to expand. These large, swelling stars are known as red giants.

The red giant phase is actually a prelude to a star shedding its outer layers and becoming a small, dense body called a white dwarf. White dwarfs cool for billions of years.

Some, if they exist as part of a binary star system , may gather excess matter from their companion stars until their surfaces explode, triggering a bright nova.

Eventually all white dwarfs go dark and cease producing energy. At this point, which scientists have yet to observe, they become known as black dwarfs.

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