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Research Group SAGE
Abstract:
From its surface properties it can be di
ffi
cult 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 e
ff
ective 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 (
ν
max
, frequency of maximum oscillation power; and
∆
ν
, frequency spacing between modes of the
same degree and consecutive radial orders) as well as e
ff
ective 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.
