| Astrophysics (Index) | About |
A brown dwarf (BD) is a star-like object which has insufficient mass to sustain fusion (the hydrogen-burning minimum mass aka HBMM) in the manner of main sequence stars ("stable fusion", i.e., of 1hydrogen), but with enough to trigger deuterium burning (the deuterium-burning minimum mass aka DBMM). This range is roughly 13 to 75 Jupiter masses, which is taken as their standard nominal mass-range. They can have an effective temperatures (Teff) ranging from 250 K to 3000 K, and any of the spectral classes, M (M dwarf), L (L dwarf), T (T dwarf), or Y (Y dwarf). They cool over the course of their life, so their spectral classification evolves, which presents a mass/age degeneracy: a young brown dwarf within the lower end of the mass range has a Teff (and spectral class) identical to that of more massive brown dwarfs that are sufficiently older. (Note that there isn't complete consistency regarding whether the term star is meant to include brown dwarfs; it likely depends upon the context, the subdiscipline, and/or the writer.)
The coolest main sequence stars are within the hotter end of the brown-dwarf range, and the classifications M and L can be hydrogen burning stars. Also, many planets are warmer than 250 K. Consequently, even with the spectral class and absolute magnitude determined, it is not clear whether or not it is a brown dwarf: its mass is an additional clue, allowing it to be (nominally) classified as a planet, a brown dwarf, or a star.
The early-established observables used to identify brown dwarfs, as opposed to main sequence stars, were the presence of lithium and/or methane (Main sequence stars generally burn their lithium early, thus its presence is a sign that the star has never burned hydrogen). The first observed brown dwarf was identified as such in 1995. As of 2015, thousands of brown dwarfs are known.
The mass criteria (13 to 75 Jupiter masses) is an imperfect indicator of whether the object burns hydrogen, deuterium, or nothing: this also depends on the constituents of the object (i.e., metallicity). It is thought that brown dwarfs actually can range from 10 to 90 Jupiter masses. The 13-75 range is at best suitable for quick or preliminary classification, a range within which brown dwarf is currently considered the most likely possibility.
Brown dwarfs' rotation periods are generally hours, typical of a planet, rather than multiple days, typical of a star. They lack stars' phases of stellar wind, which reduces a star's angular momentum. Also, they grow smaller as they cool, boosting their rotation.
There is a similarity between brown dwarfs and giant planets, such as Jupiter; both are basically hydrogen and helium, as are main sequence stars. Both are presumed to compress their hydrogen at the core to the point that it is electron degenerate matter (metallic hydrogen) without achieving a sufficient temperature/density combination to ignite the hydrogen. But star formation and planet formation theories are decidedly different: the concept of brown dwarfs grew from the idea that there would be occasions when the star formation process would not accumulate enough mass. Jupiter is presumed to have formed subsequent to the Sun, from the solar nebula and there are presumably differences between such a giant planet and such a failed star. Stars do often form in binary pairs and the fact that the object is orbiting a star is insufficient criteria. Modeling brown dwarfs and giant planets has the extra complication (over modeling stars) of the possibility of clouds in the atmosphere.
The terms black dwarf, planetar and substar were also used for brown dwarfs in the 1960s/1970s before a consensus developed regarding the term.
(The term black dwarf is currently used for far-future white dwarfs, to describe them after they cool to a more planet-like temperature.)