STELLAR VARIABILITY OF THE EXOPLANET HOSTING STAR HD 63454
- NASA Exoplanet Science Institute, Caltech, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125 (United States)
- Department of Astronomy and Space Science, Sejong University, 143-747 Seoul (Korea, Republic of)
- ESO, Karl-Schwarzschild Strasse, 2, Garching (Germany)
- Observatoire de Geneve, Universite de Geneve, 51 ch.des Maillettes, 1290 Sauverny (Switzerland)
- Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802 (United States)
Of the hundreds of exoplanets discovered using the radial velocity (RV) technique, many are orbiting close to their host stars with periods less than 10 days. One of these, HD 63454, is a young active K dwarf which hosts a Jovian planet in a 2.82 day period orbit. The planet has a 14% transit probability and a predicted transit depth of 1.2%. Here we provide a re-analysis of the RV data to produce an accurate transit ephemeris. We further analyze 8 nights of time series data to search for stellar activity both intrinsic to the star and induced by possible interactions of the exoplanet with the stellar magnetospheres. We establish the photometric stability of the star at the 3 mmag level despite strong Ca II emission in the spectrum. Finally, we rule out photometric signatures of both star-planet magnetosphere interactions and planetary transit signatures. From this we are able to place constraints on both the orbital and physical properties of the planet.
- OSTI ID:
- 21579958
- Journal Information:
- Astrophysical Journal, Vol. 737, Issue 2; Other Information: DOI: 10.1088/0004-637X/737/2/58; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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