Supernova

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A supernova is a star that, in matter of days, increases its brightness drastically, making it appear as if a "new" star was born (hence "nova"). The "super" part is to distiguish it from a nova, which also involves a star increasing in brightness, though to a lesser extent and through a much different mechanism.

Astronomers have classified supernovae in several classes, according to the lines of different elements that appear in their spectra.

The first element for division is the presence or absence of a line from hydrogen. If a supernova's spectrum does not contain a hydrogen line, it type I, otherwise type II.

Among those groups, there are subdivisions according to the presence of other lines.

Type Ia: They don't have helium, and present a line belonging to silicon. They are generally thought to be caused by the explosion of a white dwarf, at or close to the Chandrasekhar limit.

One possibility is that the white dwarf was orbiting a moderately massive star. The dwarf pulls matter from its companion to the point that it reaches the Chandrasekhar limit. The dwarf collapses into a neutron star or black hole, and the collapse causes the remaining carbon and oxygen atoms in it to fuse. This fusion produces a shockwave, and the dwarf is blown to bits. This is different from the mechanism of a nova in which the white dwarf doesn't reach the Chandrasekhar limit and collapse, but merely ignites nuclear fusion in the matter it has accreted on its surface.

The increase in luminosity is given by energy liberated by the explosion, and the rather long time it takes to decline is fueled by radioactive cobalt decaying into iron.

Type Ib and Ic: These do not have the silicon line and are even less understood. They are believed to correspond to stars ending their lives (as type II), but they would have lost their hydrogen before, thus the H lines don't appear on their spectra.

Type II: A very massive star's core begins fusing iron, which uses energy instead of liberating it. When the mass of the iron core reaches the Chandrasekhar limit (this takes only a matter of days), it decays spontaneously into neutrons and becomes much smaller. A tremendous burst of neutrinos is produced, removing energy from the star. Through a process that is not well understood some of the energy liberated in the neutrino burst is transfered to the outer layers of the star. When the shock wave reaches the surface of the star several hours later, there is a massive increase in brightness. The core of the star may become a neutron star or a black hole, depending on its mass, although because of the lack of understanding of the processes of supernova collapse, it is unclear what the cutoff mass is.

Type I supernovae are considerably brighter than Type IIs, all other things equal.


Notable supernovae:

  • 1054 - the formation of the Crab Nebula
  • Supernova 1987a - observed within hours of its start, it was the first opportunity for modern theories of supernova formation to be tested against observations.

Supernovae often leave behind supernova remnants; the study of these objects has helped to increase our knowledge of supernovae.


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