Nebula

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A nebula, which comes from the Latin word for mist or cloud,[1] is an interstellar cloud of dust, hydrogen, helium, and other gases.

An interstellar cloud is dust, plasma, or ionized gas in a galaxy. The Persian astronomer, Abd al-Rahman al-Sufi, mentioned a true nebula for the first time in his book, Book of Fixed Stars (964).[2] He said that there was a "little cloud" near the Andromeda galaxy.[3]

Origin[change | edit source]

Pelican nebula (IC5070 and IC5067)

A nebula is usually made up of hydrogen gas and plasma. It may be the first stage of a star's cycle, but it may also be one of the last stages.

Many nebulae or stars form from the gravitational collapse of gas in the interstellar medium or ISM. As the material collapses contracts, massive stars may form in the center, and their ultraviolet radiation ionises the surrounding gas, making it visible at optical wavelengths.

Examples of these types of nebulae are the Rosette nebula and the Pelican nebula. The size of these nebulae, known as HII regions, varies depending on the size of the original cloud of gas. These are sites where star formation occurs. The formed stars are sometimes known as a young, loose cluster.

Some nebulae are formed as the result of supernova explosions, the death throes of massive, short-lived stars. The materials thrown off from the supernova explosion are ionized by the energy and the compact object that it can produce. One of the best examples of this is the Crab nebula, in Taurus. The supernova event was recorded in the year 1054 and is labelled SN 1054. The compact object that was created after the explosion lies in the center of the Crab Nebula and is a neutron star.

Other nebulae may form as planetary nebulae. This is the final stage of a low-mass star's life, like Earth's Sun. Stars with a mass up to 8-10 solar masses evolve into red giants and slowly lose their outer layers during pulsations in their atmospheres. When a star has lost enough material, its temperature increases and the ultraviolet radiation it emits can ionize the surrounding nebula that it has thrown off. The nebula is 97% Hydrogen and 3% Helium with trace materials.

In the past galaxies and star clusters were also called 'nebulae'.

Types of nebulae[change | edit source]

Nebulae can be sorted by why we can see them.

Emission nebulae[change | edit source]

Emission nebulae make their own light. Usually the gases in an emission nebula are ionized. This makes them glow. Emission nebulae are usually red because they usually produce red light.

Reflection nebulae[change | edit source]

Reflection nebulae reflect light from nearby stars.

Dark nebulae[change | edit source]

Dark nebulae do not emit light or reflect light. They block the light from stars that are far away.

References[change | edit source]

  1. "Online Etymology Dictionary". etymonline.com. http://www.etymonline.com/index.php?term=nebula. Retrieved 24 September 2010.
  2. Kenneth Glyn Jones 1991. Messier's nebulae and star clusters. Cambridge University Press. p1 ISBN 0521370795
  3. Harrison, T.G. (March 1984). "The Orion Nebula — where in history is it". Royal Astronomical Society Quarterly Journal 25 (1): 70–73.

Other websites[change | edit source]