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We predict the flux and surface velocity perturbations produced byconvectively excited gravity modes (g-modes) in main sequence stars. Coreconvection in massive stars can excite g-modes to sufficient amplitudes to bedetectable with high precision photometry by Kepler and CoRoT, if the thicknessof the convective overshoot region is < 30 per cent of a pressure scale height.The g-modes manifest as excess photometric variability, with amplitudes of ~ 10micromagnitudes at frequencies ~ 10 microHz (0.8 1/d) near the solarmetallicity zero-age main sequence. The flux variations are largest for starswith M > 5 solar masses, but are potentially detectable down to M ~ 2 - 3 solarmasses. During the main sequence evolution, radiative damping decreases suchthat ever lower frequency modes reach the stellar surface and fluxperturbations reach up to ~ 100 micromagnitudes at the terminal-age mainsequence. Using the same convective excitation model, we confirm previouspredictions that solar g-modes produce surface velocity perturbations of < 0.3mm/s. This implies that stochastically excited g-modes are more easilydetectable in the photometry of massive main sequence stars than in the Sun.

The Observational Signatures of Convectively Excited Internal Gravity Modes in Main Sequence Stars