Editing Brown dwarf (section)

=== Brown dwarfs X-ray sources ===
[[File:Lp94420 duo m.jpg|thumb|300px|[[Chandra X-ray Observatory|Chandra]] image of [[LP 944-20]] before flare and during flare]]

X-ray flares detected from brown dwarfs since 1999 suggest changing [[magnetic field of celestial bodies|magnetic fields]] within them, similar to those in very-low-mass stars.  Although they do not fuse hydrogen into helium in their cores like stars, energy from the fusion of deuterium and gravitational contraction keep their interiors warm and generate strong magnetic fields.  The interior of a brown dwarf is in a rapidly boiling, or convective state. When combined with the rapid rotation that most brown dwarfs exhibit, [[convection]] sets up conditions for the development of a strong, tangled [[magnetic field]] near the surface. The magnetic fields that generated the flare observed by [[Chandra X-ray Observatory|Chandra]] from [[LP 944-20]] has its origin in the turbulent magnetized [[Plasma (physics)|plasma]] beneath the brown dwarf's "surface".

Using NASA's [[Chandra X-ray Observatory]], scientists have detected X-rays from a low-mass brown dwarf in a multiple star system.<ref name=Williams>{{cite web |date=April 14, 2003 |title=X-rays from a Brown Dwarf's Corona |url=http://www.williams.edu/Astronomy/jay/chapter18_etu6.html |access-date=March 19, 2010 |archive-url=https://web.archive.org/web/20101230000830/http://www.williams.edu/Astronomy/jay/chapter18_etu6.html |archive-date=December 30, 2010 |url-status=dead }}</ref> This is the first time that a brown dwarf this close to its parent star(s) (Sun-like stars TWA 5A) has been resolved in X-rays.<ref name=Williams/> "Our Chandra data show that the X-rays originate from the brown dwarf's coronal plasma which is some 3 million degrees Celsius", said Yohko Tsuboi of [[Chuo University]] in Tokyo.<ref name=Williams/> "This brown dwarf is as bright as the Sun today in X-ray light, while it is fifty times less massive than the Sun", said Tsuboi.<ref name=Williams/> "This observation, thus, raises the possibility that even massive planets might emit X-rays by themselves during their youth!"<ref name=Williams/>