Variability of Kepler solar-like stars harboring small exoplanets
- NASA Ames Research Center, Moffett Field, CA 94035 (United States)
- NASA Exoplanet Science Institute, California Institute of Technology, 770 S. Wilson Ave., Pasadena, CA 91125 (United States)
- National Solar Observatory, 950 N. Cherry Ave., Tucson, AZ 85719 (United States)
- National Optical Astronomy Observatory, 950 N. Cherry Ave., Tucson, AZ 85719 (United States)
- Dept. of Astronomy, University of Washington, Seattle, WA 98195 (United States)
We examine Kepler light-curve variability on habitable zone transit timescales for a large uniform sample of spectroscopically studied Kepler exoplanet host stars. The stars, taken from Everett et al., are solar-like in their properties and each harbors at least one exoplanet (or candidate) of radius ≤2.5 R{sub e}. The variability timescale examined is typical for habitable zone planets orbiting solar-like stars and we note that the discovery of the smallest exoplanets (≤1.2 R{sub e}) with corresponding transit depths of less than ∼0.18 mmag occur for the brightest and photometrically quietest stars. Thus, these detections are quite rare in Kepler observations. Some brighter and more evolved stars (subgiants), the latter of which often show large radial velocity jitter, are found to be among the photometrically quietest solar-like stars in our sample and the most likely small planet transit hunting grounds. The Sun is discussed as a solar-like star proxy to provide insight into the nature and cause of photometric variability. It is shown that Kepler’s broad, visible light observations are insensitive to variability caused by chromospheric activity that may be present in the observed stars.
- OSTI ID:
- 22890162
- Journal Information:
- The Astronomical Journal (Online), Vol. 151, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 1538-3881
- Country of Publication:
- United States
- Language:
- English
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