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A quantitative interpretation of the observed relation between theinterstellar linear polarization curve parameters $K$ and $\lambda_{\max}$characterizing the width and the wavelength of a polarization maximum,respectively, is given. The observational data available for 57 stars locatedin the dark clouds in Taurus, Chamaeleon, around the stars $\rho$ Oph and R CrAare considered. The spheroidal particle model of interstellar dust grainsearlier applied to simultaneously interpret the interstellar extinction andpolarization curves in a wide spectral range is utilized. The observed trend $K\approx 1.7 \lambda_{\max}$ is shown to be most likely related to a growth ofdust grains due to coagulation rather than mantle accretion. The relation ofthe parameters $K$ and $\lambda_{\max}$ with an average size of silicate dustgrains is discussed.

Systematic variations of interstellar linear polarization and growth of dust grains