Supernovas Research Paper A supernova is

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A supernova is a Star that explodes. It all of a sudden increases in brightness by a factor of many one million millions, and within a few hebdomads it easy slices. In footings of the human lifetime, such detonations are rare happenings. In our Milky Way galaxy, for illustration, a supernova may be observed every few hundred old ages. Three such detonations are recorded in history: in 1054, in 1572, and in 1604.

The CRAB NEBULA consists of stuff ejected by the supernova of 1054. Such stuffs, known as supernova leftovers, are common in the celestial spheres. The supernovas observed in modern times have all occurred in other galaxies, the most distant yet holding been detected in 1988 in a galaxy 5 billion light-years off. The most interesting supernova of recent times was detected in the comparatively nearby Large MAGELLANIC CLOUD, on Feb. 23, 1987, by an uranologist at Chile’s Las Campanas Observatory. It rapidly became an object of intense survey by all the agencies available to modern uranology.

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A supernova may radiate more energy in a few years than the Sun does in 100 million old ages, and the energy expended in chuck outing stuff is much greater even than this. In many instances, including the Crab nebula supernova, the leading leftover left behind after the detonation is a NEUTRON STAR – a star merely a few kilometres in diameter holding an tremendously big denseness and dwelling chiefly of neutrons – or a PULSAR, a pulsating neutron star.

There are two common types of supernovas, called type I and type II. Type I occurs among old stars of little mass, whereas type II occurs among really immature stars of big mass. It is non known how a small-mass star can let go of the really big sums of energy needed to explicate type I supernovas. Scientists by and large believe that this must affect double star systems – two stars go arounding around each other. In such a system one of the stars is a WHITE DWARF, a little, heavy star that is near the terminal of its atomic combustion stage. After pulling affair from the comrade star for some clip, the white midget finally collapses with a great haste, going a neutron star, and chuck outing affair outward. This recoil of affair is thought to be the superno Virginia. Stars with big multitudes burn their atomic fuel really quickly. Within a million old ages or less, such stars build cores incorporating much Fe. When the Fe finally burns, energy is rapidly drained from the nucleus, and the star can non go on to back up itself against gravitation. It suffers a mighty prostration correspondent to that of a type I supernova, and the recoil causes affair to be ejected in a type II supernova detonation.

Stars stoping in this manner are typically ruddy SUPERGIANTS, but the 1 that exploded as 1987A was a bluish star, named Sanduleak, with a mass merely approximately 15 times that of the Sun. Its form of brightening and attenuation besides varied notably from that of typical type II supernovas, and an as yet unexplained “mystery topographic point ” ; appeared some clip after the detonation, seemingly near to Sanduleak’s former location. In 1989 uranologists thought that they had detected an highly fast-spinning pulsar at that location, but much further information is still needed before this determination is confirmed.

Cosmologists estimate that the Universe came into being about 15 billion old ages ago. This involved the initial creative activity of H and He. Since so atomic merger in stars has changed some of the original H and He into heavier elements ( see STELLAR EVOLUTION ) . Supernovas have played an of import function both in bring for thing the heavy elements and in chuck outing stuff back into infinite, where it has been used to do new stars and, likely, PLANETARY SYSTEMS. It is possible that one or more supernovas exploded shortly before the formation of our solar system. Elements ejected from these detonations could hold mixed with the solar nebula, finally going portion of the constructions of the Sun, the Earth, and all living things.


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