Extrapolations for the breakup periods of typical brown dwarfs older than 1 billion years range tens of minutes depending on mass and radius. The high spin rate and oblateness of 2MASS J0348−6022 places it at about 45% of its rotational stability limit, assuming a smoothly varying fluid interior. Taking into account of magnetic dynamos generated by the brown dwarf's metallic hydrogen interior, the rotational velocity threshold may be even lower and implies that 2MASS J0348−6022 may be closer to breakup than predicted. As brown dwarfs cool and age, they contract in size and spin faster so as to conserve angular momentum; theoretically rapid rotators like 2MASS J0348−6022 should eventually approach their rotational stability limit and break apart, but no such phenomena have been observed . It is possible that some unknown rotational braking mechanism may be preventing brown dwarfs from breaking up as they age.
