  Asteroseismology of Sun-like stars is undergoing rapid expansion with, for
example, new data from the CoRoT mission and continuation of ground-based
campaigns. There is also the exciting upcoming prospect of NASA's Kepler
mission, which will allow the asteroseismic study of several hundred Sun-like
targets, in some cases for periods lasting up to a few years. The seismic mode
parameters are the input data needed for making inference on stars and their
internal structures. In this paper we discuss the ease with which it will be
possible to extract estimates of individual mode parameters, dependent on the
mass, age, and visual brightness of the star. Our results are generally
applicable; however, we look at mode detectability in the context of the
upcoming Kepler observations. To inform our discussions we make predictions of
various seismic parameters. To do this we use simple empirical scaling
relations and detailed pulsation computations of the stochastic excitation and
damping characteristics of the Sun-like p modes. The issues related to
parameter extraction on individual p modes discussed here are mode
detectability, the detectability and impact of stellar activity cycles, and the
ability to measure properties of rotationally split components, which is
dependent on the relative importance of the rotational characteristics of the
star and the damping of the stochastically excited p modes.
