The anomalous tail of Comet Kohoutek is studied on the basis of the dust-tail theory formulated by Finson and Probstein for the case of negligibly small emission velocities. Theoretical photometric profiles of about 170 specific models, calculated on various assumptions regarding the distribution of particle sizes and the rate of variation of dust production with heliocentric distance, are compared with the observed behavior of the anti-tail. Although no precise measurements of the light distribution in the anti-tail are available at present, its reported descriptions appear to be sufficient for tentative conclusions that there was a substantial excess of heavy particles (on the order of 0.1 to 1 mm in size) in the anti-tail and that the particle emission flux of dust from Kohoutek may have been one order of magnitude higher than that of Comets Arend-Roland and Bennett. The emission rate of dust varied in inverse proportion to the fourth power of heliocentric distance far from the Sun, less steeply nearer the Sun, and leveled off at 0.2AU from the Sun. The onset of the appreciable dust production is found to have taken place near 4 AU from the Sun, more than 200 days before perihelion. The low slope of the size-distribution function is interpreted as possible evidence for a significant loss in radius of the dust particles due to evaporation near the Sun. The latent heat of vaporization of the particle material is estimated at 40 kcal/mole or more from the difference between the observed and the expected “intrinsic” values of the population index of the particle mass distribution. Shortly after perhelion the energy emitted in the D doublet by sodium atoms released from evaporating particles may have accounted for the considerable brightness of the anti-tail at that time, whereas later its brightness was due to particle scattering of solar light.