Light curves for V2384 Orionis in three infrared bands. Representative error bars are shown in violet. Plotted from data published by Gómez Maqueo Chew et al. (2009)[4]
The pair orbit each other with a period of 9.8 days, and are about 60 and 38 times the mass of Jupiter, respectively. The system is very young, at an age of about 1 million years, so the brown dwarfs have yet to cool; they are M-type objects with temperatures comparable to red dwarf stars, and they are inflated in size to over half the radius of the Sun.[4][6] The primary is observed to rotate with a period of 3.3 days and the secondary 14 days, indicating that they have not yet become tidally locked to each other.[4]
Unexpectedly, the less massive (secondary) brown dwarf is the hotter of the pair.[6][2] Possible explanations for this temperature reversal include the two brown dwarfs differing slightly in age;[2] strong magnetic fields on the primary inhibiting convection,[2] supported by the primary's observed fast rotation and strong hydrogen-alpha emission;[7] large starspots on the primary,[4] though this was found to be unsupported by evidence;[8] and tidal heating, which is unlikely to be solely responsible for the temperature reversal.[9]
^Czesla, S.; Schneider, P. C.; Schmitt, J. H. M. M. (December 2008). "Discovery of X-ray emission from the eclipsing brown-dwarf binary 2MASS J05352184-0546085". Astronomy & Astrophysics. 491 (3): 851–854. doi:10.1051/0004-6361:200810818.
