Brown dwarf

From TFC Galactopedia

Brown dwarfs are sub-stellar objects that never fuse hydrogen into helium in their cores, as do stars on the main sequence. They do fuse deuterium.

A useful criterion for telling brown dwarfs from low mass stars is obtained through testing for lithium, which is generally present in the former and not in the latter. Stars, which achieve high temperature necessary for fusing hydrogen, rapidly deplete their lithium. This occurs by a collision of lithium 7 and a proton producing two helium 4 nuclei. The temperature necessary for this reaction is just below the temperature necessary for hydrogen fusion. Convection in the stars ensures that lithium in the whole volume of the star is depleted, resulting in an easily observable change in the star spectral lines relative to those of brown dwarfs.

Brown dwarfs continue to glow in the red and infrared after their deuterium is exhausted. This glow is from the leftover heat generated by their formation and by the earlier deuterium and lithium fusion. The atmospheres of known brown dwarfs range over temperatures from about 800 to 2500 celsius. All brown dwarfs cool over time; more massive objects cool more slowly than lower mass objects.

Source Note

• The original version of this article comes from Wikipedia, the free encyclopedia (http://en.wikipedia.org/wiki/Main_Page).