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Radial-velocity (RV) jitter due to intrinsic stellar variability introduceschallenges when characterizing exoplanet systems, particularly when studyingsmall (sub-Neptune-sized) planets orbiting solar-type stars. In this Letter wepredicted for dwarfs and giants the jitter due to stellar oscillations, whichin velocity have much larger amplitudes than noise introduced by granulation.We then fitted the jitter in terms of the following sets of stellar parameters:(1) Luminosity, mass, and effective temperature: the fit returns precisions(i.e., standard deviations of fractional residuals) of 17.9% and 27.1% fordwarfs and giants, respectively. (2) Luminosity, effective temperature, andsurface gravity: The precisions are the same as using the previous parameterset. (3) Surface gravity and effective temperature: we obtain a precision of22.6% for dwarfs and 27.1% for giants. (4): Luminosity and effectivetemperature: the precision is 47.8% for dwarfs and 27.5% for giants. Our methodwill be valuable for anticipating the radial-velocity stellar noise level ofexoplanet host stars to be found by the TESS and PLATO space missions, and thuscan be useful for their follow-up spectroscopic observations. We providepublicly available code (https://github.com/Jieyu126/Jitter) to set a prior forthe jitter term as a component when modeling the Keplerian orbits of theexoplanets.

Predicting radial-velocity jitter induced by stellar oscillations based on Kepler data