  From its surface properties it can be difficult to determine whether a
red-giant star is in its helium-core-burning phase or only burning hydrogen in
a shell around an inert helium core. Stars in either of these stages can have
similar effective temperatures, radii and hence luminosities, i.e. they can be
located at the same position in the Hertzsprung-Russell diagram.
Asteroseismology -- the study of the internal structure of stars through their
global oscillations -- can provide the necessary additional constraints to
determine the evolutionary states of red-giant stars. Here, we present a method
that uses grid-based modelling based on global asteroseismic properties
($\nu_{\rm max}$, frequency of maximum oscillation power; and $\Delta\nu$,
frequency spacing between modes of the same degree and consecutive radial
orders) as well as effective temperature and metallicity to determine the
evolutionary phases. This method is applicable even to timeseries data of
limited length, although with a small fraction of miss-classifications.
