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Supernova 1987A
"After" and "Before" pictures of Supernova 1987A

The above two photographs are of the same part of the sky. The photo on the left was taken in 1987 during the supernova explosion of SN 1987A, while the right hand photo was taken beforehand. Supernovae are one of the most energetic explosions in nature, equivalent to the power in a 1028 megaton bomb (i.e., a few octillion nuclear warheads).

Types of Supernovae

Supernovae are divided into two basic physical types:

Type Ia. These result from some binary star systems in which a carbon-oxygen white dwarf is accreting matter from a companion. (What kind of companion star is best suited to produce Type Ia supernovae is hotly debated.) In a popular scenario, so much mass piles up on the white dwarf that its core reaches a critical density of 2 x 109 g/cm3. This is enough to result in an uncontrolled fusion of carbon and oxygen, thus detonating the star.

Type II. These supernovae occur at the end of a massive star's lifetime, when its nuclear fuel is exhausted and it is no longer supported by the release of nuclear energy. If the star's iron core is massive enough, it will collapse and become a supernova.

However, these types of supernovae were originally classified based on the existence of hydrogen spectral lines: Type Ia spectra do not show hydrogen lines, while Type II spectra do.

In general this observational classification agrees with the physical classification outlined above, because massive stars have atmospheres that are made of mostly hydrogen, while white dwarf stars are bare. However, if the original star was so massive that its strong stellar wind had already blown off the hydrogen from its atmosphere by the time of the explosion, then it too will not show hydrogen spectral lines. These supernovae are often called Type Ib supernovae, despite really being part of the Type II class of supernovae. Looking at this discrepancy between our modern classification, which is based on a true difference in how supernovae explode, and the historical classification, which is based on early observations, one can see how classifications in science can change over time as we better understand the natural world.

What causes a star to blow up?

Gravity gives the supernova its energy. For Type II supernovae, mass flows into the core by the continued formation of iron from nuclear fusion. Once the core has gained so much mass that it cannot withstand its own weight, the core implodes. This implosion can usually be brought to a halt by neutrons, the only things in nature that can stop such a gravitational collapse. Even neutrons sometimes fail depending on the mass of the star's core. When the collapse is abruptly stopped by the neutrons, matter bounces off the hard iron core, thus turning the implosion into an explosion.

For a Type Ia supernova, the energy comes from the runaway fusion of carbon and oxygen in the core of a white dwarf.

Where does the core go?

When the core is less massive than about 5 solar masses, the neutrons are successful in halting the collapse of the star creating a neutron star. Neutron stars can sometimes be observed as pulsars or X-ray binaries.

When the core is more massive (Mcore > ~ 5 solar masses), nothing in the known universe is able to stop the core collapse, so the core completely falls into itself, creating a black hole, an object so dense that even light cannot escape its gravitational grasp.

To understand the phenomenon of core collapse better, consider an analogy to a rocket escaping Earth's gravity. According to Newton's law of gravity, the energy it takes to completely separate two things is given by:

E = G M m / r

where G is the Gravitational constant, M is the mass of Earth, m is the mass of the rocket and r is the distance between them (the radius of Earth). When the rocket is shot off at a given velocity v, its energy is:

E = 1/2 m v2

For the rocket to escape the Earth's gravitational field, this energy must be as least as great as the gravitational energy described in the first equation. Thus, to determine if the rocket will completely break free from the Earth's grasp, we set the two equations equal to one another and solve for v:

v = ( 2 G M / r )1/2

This result is called the escape velocity. For the Earth, the escape velocity is 11 km/sec.

Next imagine a star's central core in the role of the Earth in the above analogy. Consider what would happen if during the core collapse, the central core became so dense (i.e., the radius became very small while its mass stays the same) that something would have to travel faster than light to escape. Whenever this phenomenon occurs (i.e., Mcore > ~ 5 solar masses), the supernova creates a black hole from the core of the original star. Now the escape velocity is greater than the speed of light, which is 300,000 km/sec.

Where does most of the star go?

The core is only the very small center of an extremely large star that for many millions of years had been making many (but not all) of the elements that we find here on Earth. When a star's core collapses, an enormous blast wave is created with the energy of about 1028 mega-tons. This blast wave plows the star's atmosphere into interstellar space, propelling the elements created in the explosion outward as the star becomes a supernova remnant.

Are we made of stardust?

Many of the more common elements were made through nuclear fusion in the cores of stars, but many of the rarer elements were not. Because nuclear fusion reactions that make elements heavier than iron require more energy than they give off, such reactions do not occur under stable conditions in typical stars. On the other hand, supernovae are not stable, so they can make these heavy elements beyond iron.

In addition to making elements, supernovae scatter the elements that are made by both the star and supernova out into the interstellar medium. These are the elements that make up stars, planets and everything on Earth, including our bodies.

How often do supernovae occur?

Although many supernovae have been seen in nearby galaxies, supernova explosions are relatively rare events in our own galaxy, happening once a century or so on average. The last nearby supernova explosion occurred in 1680, It was thought to be just a normal star at the time, but it caused a discrepancy in the observer's star catalogue, which historians finally resolved 300 years later, after the supernova remnant (Cassiopeia A) was discovered and its age estimated. Before 1680, the two most recent supernova explosions were observed by the great astronomers Tycho Brahe and Johannes Kepler in 1572 and 1604 respectively.

In 1987, there was a supernova explosion in the Large Magellanic Cloud, a companion galaxy to the Milky Way. Supernova 1987A, which is shown at the top of the page, is close enough to continuously observe as it changes over time, thus greatly expanding astronomers' understanding of this fascinating phenomenon.

More information

A good book written for the non-scientist is:
The Supernova Story, by Laurence A. Marschall, ©1988, Plenum Press, ISBN:0306429551.

Last Modified: January 2011


A service of the High Energy Astrophysics Science Archive Research Center (HEASARC), Dr. Alan Smale (Director), within the Astrophysics Science Division (ASD) at NASA/GSFC

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