  We propose a new method of the automated identification of current sheets
(CSs) that represents a formalization of the visual inspection approach
employed in case studies. CSs are often identified by eye via the analysis of
characteristic changes in the interplanetary magnetic field (IMF) and plasma
parameters. Known visual and semi-automated empirical methods of CS
identification are exact but do not allow a comprehensive statistical analysis
of CS properties. Existing automated methods partially solve this problem.
Meanwhile, these methods suggest an analysis of variations of the IMF and its
direction only, being based on Taylor's hypothesis applicable mainly to
turbulent plasmas but not to CSs of all kinds. In our three-parameter empirical
method, we employ both the solar wind plasma and IMF parameters to identify CSs
of various types. Derivatives of the IMF strength, the plasma beta and the
ratio of the Alfv'en speed VA to the solar wind speed V taken with the
one-second cadence are used. We find that the CS daily rate R correlates with
the solar wind temperature T rather than with V and is proportional to the sum
of the kinetic and thermal energy density ~ V2(N+5N')+10T(N+N'), where
N'=2cm^-3 is the background level of the solar wind density N. Maxima of R are
associated with stream/corotating interaction regions and interplanetary mass
ejection sheaths. A multiyear list of CSs identified at 1 AU can be found at
https://csdb.izmiran.ru
