The V = 4.48 F4 main-sequence star \theta Cyg is the brightest star observable in the Kepler spacecraft field of view .
Short-cadence ( 58.8 s ) photometric data were obtained by Kepler during 2010 June - September .
Preliminary analysis shows solar-like oscillations in the frequency range 1200 - 2500 \mu Hz .
To interpret these data and to motivate further observations , we use observational constraints from the literature to construct stellar evolution and pulsation models for this star .
We compare the observed large frequency separation of the solar-like oscillations with the model predictions , and discuss the prospects for \gamma Doradus-like g-mode pulsations , given the observational constraints .
We discuss the value of angular diameter measurements from optical interferometry for constraining stellar properties and the implications for asteroseismology .