  The Kepler space telescope yielded unprecedented data for the study of
solar-like oscillations in other stars. The large samples of multi-year
observations posed an enormous data analysis challenge that has only recently
been surmounted. Asteroseismic modeling has become more sophisticated over
time, with better methods gradually developing alongside the extended
observations and improved data analysis techniques. We apply the latest version
of the Asteroseismic Modeling Portal (AMP) to the full-length Kepler data sets
for 57 stars and the Sun, comprising planetary hosts, binaries, solar-analogs,
and active stars. From an analysis of the derived stellar properties for the
full sample, we identify a variation of the mixing-length parameter with
atmospheric properties. We also derive a linear relation between the stellar
age and a characteristic frequency separation ratio. In addition, we find that
the empirical correction for surface effects suggested by Kjeldsen and
coworkers is adequate for solar-type stars that are not much hotter (Teff <
6200 K) or significantly more evolved (logg > 4.2, <Delta_nu> > 80 muHz) than
the Sun. Precise parallaxes from the Gaia mission and future observations from
TESS and PLATO promise to improve the reliability of stellar properties derived
from asteroseismology.
