Editing Brown dwarf (section)

=== Deuterium fusion ===
The discovery of [[deuterium burning]] down to {{solar mass|0.013|link=yes}} ({{val|13.6|u=[[Jupiter mass|''M''{{sub|J}}]]}}) and the impact of dust formation in the cool outer [[atmosphere]]s of brown dwarfs in the late 1980s brought these theories into question. However, such objects were hard to find because they emit almost no visible light. Their strongest emissions are in the [[infrared]] (IR) spectrum, and ground-based IR detectors were too imprecise at that time to readily identify any brown dwarfs.

Since then, numerous searches by various methods have sought these objects. These methods included multi-color imaging surveys around field stars, imaging surveys for faint companions of [[main sequence|main-sequence]] dwarfs and [[white dwarfs]], surveys of young [[star clusters]], and [[radial velocity]] monitoring for close companions.