X-ray Astronomy: Supernovae and their remnants - Introduction
Animation of a supernova explosion, ending in a pulsing neutron star
SupernovaeA supernova (the plural is supernovae) is the explosion of a star. They are extremely important for understanding our Galaxy. They heat up the interstellar medium, distribute heavy elements throughout the Galaxy, and accelerate cosmic rays. But what causes a star to explode? And is there more than one type of supernova?
Indeed, there seems to be two distinct types of supernovae -- those which occur for a single massive star and those which occur because of mass transfer onto a white dwarf in a binary system. As you will see, however, it is only what gets the process started toward the explosion which differs between the two types.
Supernovae from Single, Massive Stars
|The Life Cycle of a Massive Star|
|Cygnus Loop in X-rays
||Crab Nebula in X-rays|
All that remains of the original star is a small, super-dense core composed almost entirely of neutrons -- a neutron star. Or, if the original star is very massive indeed (say 15 or more times the mass of our Sun), even the neutrons cannot survive the core collapse...and a black hole forms.
The hot material given off by the supernova, the radioactive isotopes, and the free electrons moving in the strong magnetic field of the neutron star... all of these things produce X-rays and gamma rays. These high-energy photons are used by astrophysicists to study the phenomena of neutron stars and supernovae.
A White Dwarf Goes ThermonuclearAnother type of supernova involves the sudden explosion of a white dwarf star in a binary star system. A white dwarf is the endpoint for stars of up to about 8 times that of the Sun. The remaining white dwarf has a mass less than 1.4 times the mass of the Sun, and is about the size of the Earth.
In a binary star system, the white dwarf's companion star is often a red giant. The stars may be close enough to each other and the red giant large enough, that material may flow from the red giant onto the white dwarf.
Should the in-falling matter from the companion star cause the white dwarf to approach a mass of 1.4 times that of the Sun (a mass called the Chandrasekhar limit after the scientist who discovered it), the pressure at the center will exceed the threshold for the carbon and oxygen nuclei to start to fuse uncontrollably. This results in a thermonuclear detonation of the entire star. Nothing is left behind, except whatever elements were left over from the white dwarf or forged in the supernova blast. Among the new elements is radioactive nickel, which liberates huge amounts of energy, including visible light. The evolution of these supernovae tend to all be similar.
Last Modified: September 2009