A method for detecting voids in the galaxy distribution is presented . Using this method , we have identified 732 voids with a radius of the seed sphere R _ { seed } > 4.0 h ^ { -1 }  Mpc in a volume-limited sample of galaxies from the southern part of the 2dFGRS survey . 110 voids with R _ { seed } > 9.0 h ^ { -1 }  Mpc have a positive significance . The mean volume of such voids is 19 \cdot 10 ^ { 3 } h ^ { -3 }  Mpc ^ { 3 } . Voids with R _ { seed } > 9.0 h ^ { -1 }  Mpc occupy 55 % of the sample volume . We construct a dependence of the volumes of all the identified voids on their ranks and determine parameters of the galaxy distribution . The dependence of the volume of voids on their rank is consistent with a fractal model ( Zipf’s power law ) of the galaxy distribution with a fractal dimension D \approx 2.1 ( given the uncertainty in determining the dimension using our method and the results of a correlation analysis ) up to scales of 25 h ^ { -1 }  Mpc with the subsequent transition to homogeneity . The directions of the greatest elongations of voids and their ellipticities ( oblateness ) are determined from the parameters of equivalent ellipsoids . The directions of the greatest void elongations have an enhanced concentration to the directions perpendicular to the line of sight .