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Calibration of the period-luminosity relation (PLR) for Cepheids has alwaysbeen one of the biggest goals of stellar astronomy. Among a considerable numberof different approaches, the Baade-Becker-Wesselink (BBW) method stands in theforeground as one of the most universal and precise methods. We present a newrealization of the BBW method which is considered to be the generalization ofsurface brightness (\citealt{Barnes+Evans+1976}) and \cite{Balona+1977}approaches first proposed by \cite{Rastorguev+Dambis+2010} and described in\cite{Paper1}. One of the main features of this method is using measuredeffective temperature variations to determine the main parameters of Cepheid,such as distance, radius, luminosity, colour excess, intrinsic colour. We applythis method to 45 Cepheids of Northern sky, for which multiphase temperaturedata are available. We take into account the effect of shock waves, whosepresence in stellar atmosphere distorts the observational data and thecalibrations used in this work. Within $0.0-0.87$ phase interval we derived PLrelation $<M_V>_I=-(2.67 \pm 0.17)\cdot logP - (1.58 \pm 0.16)$. It was used tocalculate the distances, rotation curve and kinematical parameters of thesample of 435 Cepheids with GAIA DR2 proper motions.

The period-luminosity relation for Cepheids derived from multiphase temperature measurements and Cepheids kinematics based on GAIA DR2 data