  Forecasting the arrival time of CMEs and their associated shocks is one of
the key aspects of space weather research. One of the commonly used models is,
due to its simplicity and calculation speed, the analytical drag-based model
(DBM) for heliospheric propagation of CMEs. DBM relies on the observational
fact that slow CMEs accelerate whereas fast CMEs decelerate, and is based on
the concept of MHD drag, which acts to adjust the CME speed to the ambient
solar wind. Although physically DBM is applicable only to the CME magnetic
structure, it is often used as a proxy for the shock arrival. In recent years,
the DBM equation has been used in many studies to describe the propagation of
CMEs and shocks with different geometries and assumptions. Here we give an
overview of the five DBM versions currently available and their respective
tools, developed at Hvar Observatory and frequently used by researchers and
forecasters. These include: 1) basic 1D DBM, a 1D model describing the
propagation of a single point (i.e. the apex of the CME) or concentric arc
(where all points propagate identically); 2) advanced 2D self-similar cone DBM,
a 2D model which combines basic DBM and cone geometry describing the
propagation of the CME leading edge which evolves self-similarly; 3) 2D
flattening cone DBM, a 2D model which combines basic DBM and cone geometry
describing the propagation of the CME leading edge which does not evolve
self-similarly; 4) DBEM, an ensemble version of the 2D flattening cone DBM
which uses CME ensembles as an input and 5) DBEMv3, an ensemble version of the
2D flattening cone DBM which creates CME ensembles based on the input
uncertainties. All five versions have been tested and published in recent years
and are available online or upon request. We provide an overview of these five
tools, of their similarities and differences, as well as discuss and
demonstrate their application.
