1999PASP..111.1529D

Up to now, the occurrence of planetary systems around brown dwarfs has not been studied in detail. However, there is no reason to exclude the occurrence of planets around brown dwarfs. Moreover, their smaller mass with respect to normal stars makes more prominent the effects due to the presence of planets, allowing in principle the identification of planets with smaller masses (i.e., Earth-like planets). In this paper we present a feasibility study of the detection of planetary companions around the brown dwarf Gliese 229B (M=0.025-0.055 M_☉) using near-infrared high-resolution spectroscopy to measure radial velocity variations. Issues concerning the intrinsic stability of brown dwarfs as well as instrument requirements are considered.