Brown dwarfs are substellar objects too low in mass to sustain hydrogen-1 fusion reactions in their cores, unlike main-sequence stars, which can. They occupy the mass range between the heaviest gas giants and the lightest stars, with an upper limit around 75[1] to 80 Jupiter masses (). Brown dwarfs heavier than about 13 are thought to fuse deuterium and those above ~65 , fuse lithium as well.[2]
However, for some years now there has been debate concerning what criterion to use for defining the separation between a brown dwarf and a giant planet at very low brown dwarf masses (~13 Jupiter masses).[3] One school of thought is based on formation, and another on interior physics.[3]
Dwarfs are categorized by spectral classification, with the major types being M, L, T, and Y.[3] Despite their name, most brown dwarfs would appear magenta to the human eye.[3]
Another debate is whether brown dwarfs are required to have experienced fusion at some point in their history. Some planets are known to orbit brown dwarfs: 2M1207b, MOA-2007-BLG-192Lb, and 2MASS J044144b. Brown dwarfs may have fully convective surfaces and interiors, with no chemical differentiation by depth.[4]