  Asteroseismology of solar-type stars has entered a new era of large surveys
with the success of the NASA \textit{Kepler} mission, which is providing
exquisite data on oscillations of stars across the Hertzprung-Russell (HR)
diagram. From the time-series photometry, the two seismic parameters that can
be most readily extracted are the large frequency separation ($\Delta\nu$) and
the frequency of maximum oscillation power ($\nu_\mathrm{max}$). After the
survey phase, these quantities are available for hundreds of solar-type stars.
By scaling from solar values, we use these two asteroseismic observables to
identify for the first time an evolutionary sequence of 1-M$_\odot$ field
stars, without the need for further information from stellar models. Comparison
of our determinations with the few available spectroscopic results shows an
excellent level of agreement. We discuss the potential of the method for
differential analysis throughout the main-sequence evolution, and the
possibility of detecting twins of very well-known stars.
