Everything about Carbon Detonation totally explained
Carbon detonation is a violent re-ignition of
thermonuclear fusion in a
dead star, which produces a
Type Ia supernovae.
Process
A
white dwarf undergoes
carbon detonation only if it has a normal
binary companion which is close enough to the dwarf star to dump sufficient amounts of matter onto the dwarf, expelled during the process of the companion's own late stage
evolution.
If the companion supplies enough matter to the dead star, the white dwarf's internal pressure and temperature will rise high enough to fuse the previously unfusable
carbon in the white dwarf's core. Carbon detonation generally occurs when the accreted matter pushes the white dwarf's mass close to the
Chandrasekhar limit of roughly 1.4
solar masses.
Computer simulations show that the fusion front proceeds as a series of turbulent, expanding "bubbles" that exhibit
Rayleigh-Taylor instability. The turbulence of the unstable fusion front makes it ragged, and the high surface area of the ragged front results in an extremely rapid "burn", known as a "thermonuclear flame". This rapid "burn" erupts explosively through the dwarf star's surface, which is seen as a type Ia supernova.
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