The period-luminosity relation for Cepheids derived from multiphase
  temperature measurements and Cepheids kinematics based on GAIA DR2 data
  Calibration of the period-luminosity relation (PLR) for Cepheids has always
been one of the biggest goals of stellar astronomy. Among a considerable number
of different approaches, the Baade-Becker-Wesselink (BBW) method stands in the
foreground as one of the most universal and precise methods. We present a new
realization of the BBW method which is considered to be the generalization of
surface 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 measured
effective temperature variations to determine the main parameters of Cepheid,
such as distance, radius, luminosity, colour excess, intrinsic colour. We apply
this method to 45 Cepheids of Northern sky, for which multiphase temperature
data are available. We take into account the effect of shock waves, whose
presence in stellar atmosphere distorts the observational data and the
calibrations used in this work. Within $0.0-0.87$ phase interval we derived PL
relation $<M_V>_I=-(2.67 \pm 0.17)\cdot logP - (1.58 \pm 0.16)$. It was used to
calculate the distances, rotation curve and kinematical parameters of the
sample of 435 Cepheids with GAIA DR2 proper motions.
