  We propose a scenario to form low-mass, single, slow rotating white dwarfs
from a solar-like star accompanied by a massive planet, or a brown dwarf, in a
relatively close orbit (e.g. HD 89707). Such white dwarfs were recently found
by Maxted & Marsh (1998). When the solar-like star ascends the giant branch it
captures the planet and the subsequent spiral-in phase expels the envelope of
the giant leaving a low-mass helium white dwarf remnant. In case the planet
evaporizes, or fills its own Roche-lobe, the outcome is a single undermassive
white dwarf. The observed distribution of planetary systems supports the
applicability of this scenario.
