From the kinematically unbiased sample of halo stars, the local mass density of halo dwarfs is estimated as $6.0{sim}6.3{ imes}10^{-4}m_{odot}/pc^3$ by adopting a color-magnitude relation and a mass-luminosity relation. The derived halo mass density is not much different from the results of previous studies, which were derived from the kinematically biased sample of halo stars. Therefore it is confirmed that the local mass density of halo stars is far less than that required by Ostriker-Peebles to stabilize the galactic disk against barlike instabilities.