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This Earth-sized sphere, consisting mainly of carbon and oxygen, is incredibly dense, the most massive up to around 1.
Only something called electron degeneracy pressure, an outward pressure generated by the inability of electrons with the same spin to occupy the same state, prevents the core from complete collapse.
Because they are so dense, with such a small surface area, they take a very long time to lose heat. Once the core of a white dwarf has stopped contracting, it can exceed temperatures of around , Kelvin around , degrees Celsius and , degrees Fahrenheit.
Astronomers think that not enough time has passed since the beginning of the Universe for a white dwarf to have cooled completely. But the so-called Q-branch white dwarf stars, which constitute around 6 percent of massive white dwarfs, cool even slower than that.
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.
Massive stars eschew this evolutionary path and instead go out with a bang—detonating as supernovae. While they may appear to be swelling red giants on the outside, their cores are actually contracting, eventually becoming so dense that they collapse, causing the star to explode.
These catastrophic bursts leave behind a small core that may become a neutron star or even, if the remnant is massive enough, a black hole.
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