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Determining the ages of red-giant stars is a key problem in stellarastrophysics. One of the difficulties in this determination is to know theevolutionary state of the individual stars -- i.e. have they started to burnHelium in their cores? That is the topic of this paper. Asteroseismic dataprovide a route to achieving this information. What we present here is anhighly autonomous way of determining the evolutionary state from an analysis ofthe power spectrum of the light curve. The method is fast and efficient and canprovide results for a large number of stars. It uses the structure of thedipole-mode oscillations, which have a mixed character in red-giant stars, todetermine some measures that are used in the categorisation. It does notrequire that all the individual components of any given mode be separatelycharacterised. Some 6604 red giant stars have been classified. Of these 3566are determined to be on the red-giant branch, 2077 are red-clump and 439 aresecondary-clump stars. We do not specifically identify the low metallicity,horizontal-branch stars. The difference between red-clump and secondary-clumpstars is dependent on the manner in which Helium burning is first initiated. Wediscuss that the way the boundary between these classifications is set may leadto mis-categorisation in a small number of stars. The remaining 522 stars werenot classified either because they lacked sufficient power in the dipole modes(so-called depressed dipole modes) or because of conflicting values in theparameters.

A New Method for the Asteroseismic Determination of the Evolutionary State of Red-Giant Stars