  In the past decade, helioseismology has revolutionized our understanding of
the interior structure of the Sun. In the next decade, asteroseismology will
place this knowledge into context, by providing structural information for
dozens of pulsating stars across the H-R diagram. Solar-like oscillations have
already been detected from the ground in a few stars, and several current and
planned satellite missions will soon unleash a flood of stellar pulsation data.
Deriving reliable seismological constraints from these observations will
require a significant improvement to our current analysis methods. We are
adapting a computational method, based on a parallel genetic algorithm, to help
interpret forthcoming observations of Sun-like stars. This approach was
originally developed for white dwarfs and ultimately led to several interesting
tests of fundamental physics, including a key astrophysical nuclear reaction
rate and the theory of stellar crystallization. The impact of this method on
the analysis of pulsating white dwarfs suggests that seismological modeling of
Sun-like stars will also benefit from this approach.
