  Pulsating white dwarf stars can be used as astrophysical laboratories to
constrain the properties of weakly interacting particles. Comparing the cooling
rates of these stars with the expected values from theoretical models allows us
to search for additional sources of cooling due to the emission of axions,
neutralinos, or neutrinos with magnetic dipole moment. In this work, we derive
an upper bound to the neutrino magnetic dipole moment using an estimate of the
rate of period change of the pulsating DB white dwarf star PG 1351+489. By
comparing the theoretical rate of change of period expected for this star with
the rate of change of period with time of PG 1351+489, we assess the possible
existence of additional cooling by neutrinos with magnetic dipole moment. Our
models suggest the existence of some additional cooling in this pulsating DB
white dwarf, consistent with a non-zero magnetic dipole moment. Our upper limit
for the neutrino magnetic dipole moment is somewhat less restrictive than, but
still compatible with, other limits inferred from the white dwarf luminosity
function or from the color-magnitude diagram of the Globular cluster M5.
Further improvements of the measurement of the rate of period change of the
dominant pulsation mode of PG 1351+489 will be necessary to confirm our bound.
